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  1. T-607: Update: Adobe Acrobat, Reader, and Flash Player SWF File Processing Arbitrary Code Execution Vulnerability

    Broader source: Energy.gov [DOE]

    Update: Adobe Acrobat, Reader, and Flash Player SWF File Processing Arbitrary Code Execution Vulnerability.

  2. T-577: Security Advisory for Adobe Flash Player, Adobe Reader and Acrobat

    Broader source: Energy.gov [DOE]

    A critical vulnerability exists in Adobe Flash Player 10.2.152.33 and earlier versions (Adobe Flash Player 10.2.154.13 and earlier for Chrome users) for Windows, Macintosh, Linux and Solaris operating systems, Adobe Flash Player 10.1.106.16 and earlier versions for Android, and the Authplay.dll component that ships with Adobe Reader and Acrobat X (10.0.1) and earlier 10.x and 9.x versions of Reader and Acrobat for Windows and Macintosh operating systems.

  3. U-064: Adobe Acrobat/Reader PRC Memory Corruption Error Lets Remote Users Execute Arbitrary Code

    Broader source: Energy.gov [DOE]

    A vulnerability was reported in Adobe Acrobat/Reader, this vulnerability is being actively exploited against Windows-based systems.

  4. T-600: Security Advisory for Adobe Flash Player, Adobe Reader and Acrobat

    Broader source: Energy.gov [DOE]

    This vulnerability (CVE-2011-0611) could cause a crash and potentially allow an attacker to take control of the affected system. There are reports that this vulnerability is being exploited in the wild in targeted attacks via a Flash (.swf) file embedded in a Microsoft Word (.doc) file delivered as an email attachment, targeting the Windows platform. At this time, Adobe is not aware of any attacks via PDF targeting Adobe Reader and Acrobat. Adobe Reader X Protected Mode mitigations would prevent an exploit of this kind from executing.

  5. T-555: Adobe Acrobat and Reader Image Parsing Arbitrary Code Execution Vulnerability

    Broader source: Energy.gov [DOE]

    Critical vulnerabilities have been identified in Adobe Reader X (10.0) for Windows and Macintosh; Adobe Reader 9.4.1 and earlier versions for Windows, Macintosh and UNIX; and Adobe Acrobat X (10.0) and earlier versions for Windows and Macintosh. These vulnerabilities could cause the application to crash and potentially allow an attacker to take control of the affected system. Risk for Adobe Reader X users is significantly lower, as none of these issues bypass Protected Mode mitigations.

  6. Acrobat Settings

    Office of Energy Efficiency and Renewable Energy (EERE)

    Use these best practices for configuring Adobe Acrobat when creating PDFs. PDFs should be created with Adobe Acrobat version 9 or higher. The instructions below are for Acrobat XI. For instructions...

  7. U-146: Adobe Reader/Acrobat Multiple Vulnerabilities | Department of Energy

    Office of Environmental Management (EM)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann Jackson About1996HowFOAShowing YouNeed forUnruhDepartment ofM I C HCommands on|6: Adobe

  8. Create an ETD Using Adobe Lesson 1: Create a PDF File

    E-Print Network [OSTI]

    Carver, Jeffrey C.

    Create an ETD Using Adobe® Acrobat® Lesson 1: Create a PDF File 1 Create a PDF File #12;Create an ETD Using Adobe® Acrobat® Lesson 1: Create a PDF File 2 Tip The default settings will create an ETD. Click on the Restore Defaults button to make sure that the defaults are selected or click

  9. Acrobat XI Configuration

    Broader source: Energy.gov [DOE]

    Acrobat XI includes a number of configuration options. The following PDFs include EERE's recommended configuration for preparing standards compliant PDFs. The files also include the job settings needed.

  10. Online Proofing System 1.Corrections should be marked with the Adobe Annotation & Comment Tools below

    E-Print Network [OSTI]

    Maestripieri, Dario

    Online Proofing System 1.Corrections should be marked with the Adobe Annotation & Comment Tools-ANNOTATION TOOLS FOR ELECTRONIC PROOF CORRECTION Required software to e-Annotate PDFs: Adobe Acrobat Professional. Replace (Ins) Tool ­ for replacing text. Strikes a line through text and opens up a text box where

  11. T-622: Adobe Acrobat and Reader Unspecified Memory Corruption Vulnerability

    Broader source: Energy.gov [DOE]

    The vulnerability is due to an unspecified error in the affected software when it processes .pdf files. An unauthenticated, remote attacker could exploit this vulnerability by convincing a user to view a malicious .pdf file. When viewed, the file could trigger a memory corruption error that could allow the attacker to execute arbitrary code on the system with the privileges of the user.

  12. Adobe Acrobat Settings for Creating PDFs | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Financing ToolInternationalReportOfficeAcqguide18pt0 MarchEnergyEnergy Administrative

  13. V-157: Adobe Reader / Acrobat Multiple Vulnerabilities | Department of

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyThe U.S.Lacledeutilities. The Economics of ElectricScripting Attacks

  14. PC Windows Adobe Creative Cloud PC Windows Adobe Creative Cloud

    E-Print Network [OSTI]

    PC Windows Adobe Creative Cloud 1 PC Windows Adobe Creative Cloud 2015-05-25 1 Web Windows Adobe Creative Cloud PC | Creative Cloud https://helpx.adobe.com/jp/creative-cloud Adobe Creative Cloud 5.1 Web TTInstaller(Windows )() http://www.officesoft.gsic.titech.ac

  15. Residential California adobe : mud form

    E-Print Network [OSTI]

    Daymond, Diana Leigh

    1985-01-01

    Northern California has a rich tradition of adobe architecture . Formed with earth, defined by site, climate and use, the adobe structures exemplify a building methodology in harmony with nature and the lifestyle of it's ...

  16. VIEWING INSTRUCTIONS The following document is an Adobe Acrobat version of the 2001 BNL Groundwater

    E-Print Network [OSTI]

    Groundwater Status Report. Portions of the document have bookmarks on the left hand side of the screen'S MYSTERIES ...PROTECTING ITS FUTURE 2001 BNL GROUNDWATER STATUS REPORT June 13, 2002 Environmental Services10886 #12;2001 BNL Groundwater Status Report i 2001 BNL Groundwater Status Report TABLE OF CONTENTS

  17. V-066: Adobe Acrobat/Reader Multiple Flaws Lets Remote Users Execute

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics And Statistics » USAJobs Search USAJobs SearchWater-Saving Projects1: OracleEnergyArbitrary

  18. PC Mac OS Adobe Creative Cloud PC Mac OS Adobe Creative Cloud

    E-Print Network [OSTI]

    PC Mac OS Adobe Creative Cloud 1 PC Mac OS Adobe Creative Cloud 2015-05-25 1 Web Mac OS Adobe Creative Cloud PC | Creative Cloud https://helpx.adobe.com/jp/creative-cloud Adobe Creative Cloud 5.1 Web TTInstaller (Mac OS X )() http://www.officesoft.gsic.titech.ac.jp/pdf

  19. U-187: Adobe Flash Player Multiple Vulnerabilities

    Broader source: Energy.gov [DOE]

    Adobe released security updates for Adobe Flash Player 11.2.202.235 and earlier versions for Windows, Macintosh and Linux, Adobe Flash Player 11.1.115.8 and earlier versions for Android 4.x, and Adobe Flash Player 11.1.111.9 and earlier versions for Android 3.x and 2.x. These updates address vulnerabilities that could cause a crash and potentially allow an attacker to take control of the affected system.

  20. Adobe Solar | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmental Jump to:EAand DaltonSolar Energy LLCAdema Technologies Inc JumpAdobe Solar Jump to:

  1. V-176: Adobe Flash Player Memory Corruption Flaw Lets Remote...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    and earlier versions for Linux Adobe Flash Player 11.1.115.58 and earlier versions for Android 4.x Adobe Flash Player 11.1.111.54 and earlier versions for Android 3.x and 2.x Adobe...

  2. U-104: Adobe Flash Player Multiple Vulnerabilities

    Broader source: Energy.gov [DOE]

    Multiple vulnerabilities have been reported in Adobe Flash Player, which can be exploited by malicious people to conduct cross-site scripting attacks, bypass certain security restrictions, and compromise a user's system.

  3. T-609: Adobe Acrobat/Reader Memory Corruption Error in CoolType Library Lets Remote Users Execute Arbitrary Code

    Broader source: Energy.gov [DOE]

    A remote user can create a specially crafted PDF file that, when loaded by the target user, will trigger a memory corruption error in the CoolType library and execute arbitrary code on the target system. The code will run with the privileges of the target user.

  4. U-241: Adobe Flash Player Bugs Let Remote Users Execute Arbitrary...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    and Linux operating systems Adobe Flash Player 11.1.115.11 and earlier versions for Android 4.x Adobe Flash Player 11.1.111.10 and earlier versions for Android 3.x and 2.x Adobe...

  5. ADOBE PHOTOSHOP 5.0 Back to Contents

    E-Print Network [OSTI]

    Durand, Frédo

    Tutorial ADOBE PHOTOSHOP 5.0 Back to Contents Photo Retouching Adobe® Photoshop® provides you techniques for basic image correction by stepping you through the process of acquiring, resizing correct problems in composition and sharpen the overall focus of the image. Basic steps Most retouching

  6. ADOBE PHOTOSHOP 5.0 Back to Contents

    E-Print Network [OSTI]

    Durand, Frédo

    Tutorial ADOBE PHOTOSHOP 5.0 Back to Contents Layer Basics Adobe® Photoshop® lets you isolate flexibility in composing and revising an image. #12;LAYER BASICS PAGE 2 OF 11 In this lesson, you'll learn how about the Layers palette and layer options. #12;LAYER BASICS PAGE 3 OF 11 3 Choose File > Open. Locate

  7. ADOBE PHOTOSHOP 5.0 Back to Contents

    E-Print Network [OSTI]

    Durand, Frédo

    Tutorial ADOBE PHOTOSHOP 5.0 Back to Contents Working with Selections Learning how to select areas four basic sets of tools--the marquee, lasso, magic wand, and pen tools. In addition, you can use

  8. Policy Flashes FY 2003 | Department of Energy

    Energy Savers [EERE]

    please contact the Office of Procurement and Assistance Policy on (202) 287-1330. If a Policy Flash andor attachment is in a different format than Adobe Acrobat, the format...

  9. U-166: Adobe Shockwave Player Memory Corruption Flaws Let Remote Users Execute Arbitrary Code

    Broader source: Energy.gov [DOE]

    Multiple vulnerabilities were reported in Adobe Shockwave Player. A remote user can cause arbitrary code to be executed on the target user's system.

  10. U-136: Adobe Flash Player Lets Remote Users Execute Arbitrary Code

    Broader source: Energy.gov [DOE]

    Two vulnerabilities were reported in Adobe Flash Player. A remote user can cause arbitrary code to be executed on the target user's system.

  11. V-069: BlackBerry Tablet OS Adobe Flash Player and Samba Multiple...

    Broader source: Energy.gov (indexed) [DOE]

    OS Adobe Flash Player and Samba Multiple Vulnerabilities PLATFORM: BlackBerry Tablet Software versions 2.1.0.1032 and prior. ABSTRACT: Multiple vulnerabilities have been reported...

  12. Casas Adobes, Arizona: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmentalBowerbank,Cammack Village, Arkansas:FundMichigan:NorthCasas Adobes, Arizona: Energy

  13. T-627: Adobe Flash Player Memory Corruption | Department of Energy

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LIST OF APPLICABLEStatutory Authority SustainXSystem for Award35:Department|27: Adobe

  14. Student Traffic Court Justice Application IMPORTANT: IF YOU ARE USING A MAC, you must download Adobe Reader (http://get.adobe.com/reader/) and use it to open/save the application.

    E-Print Network [OSTI]

    Sin, Peter

    Adobe Reader (http://get.adobe.com/reader/) and use it to open/save the application. Applications saved by Email button will not work. Instead, choose File, Save As, and save the PDF to your hard drive. You may

  15. T-549: Adobe ColdFusion 9.0.1 CHF1 and earlier

    Broader source: Energy.gov [DOE]

    Cross-site scripting (XSS) vulnerability in Adobe ColdFusion before 9.0.1 CHF1 allows remote attackers to inject arbitrary web script or HTML via vectors involving a "tag script.

  16. T-569: Adobe Flash SWF File Processing Memory Corruption Remote Code Execution Vulnerability

    Broader source: Energy.gov [DOE]

    Critical vulnerabilities have been identified in Adobe Flash Player 10.1.102.64 and earlier versions for Windows, Macintosh, Linux, and Solaris. These vulnerabilities could cause the application to crash and could potentially allow an attacker to take control of the affected system.

  17. T-604: Google Chrome updated version of the Adobe Flash player

    Broader source: Energy.gov [DOE]

    The Chrome Stable channel has been updated to 10.0.648.205 for Windows, Mac, Linux and Chrome Frame. This release contains a new version of Adobe Flash 0-Day CVE-2011-0611. Update also includes a fix for a security vulnerability Critical CVE-2011-1300: Off-by-three in GPU process, CVE-2011-1301: Use-after-free in the GPU process, and CVE-2011-1302: Heap overflow in the GPU process.

  18. Adobe House 

    E-Print Network [OSTI]

    Unknown

    2011-09-05

    show that in some cases the resultant energy consumption obtained from installing high-performance windows was lower than the energy consumption of a base-case windowless house (Approximately 6% total energy savings, and 40% heating)....

  19. 2014 NERSC Achievement Award Recipient Presentations

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    PDF file Conformational change in biology: from amino acids to enzymes and molecular motors, Victor Ovchinnikov, Harvard University JainNERSCUserDay2.pdf | Adobe Acrobat PDF file...

  20. Mid-Atlantic Region Combined Heat and Power Projects

    Broader source: Energy.gov [DOE]

    DOE's CHP Technical Assistance Partnerships (CHP TAPs) have compiled a select number of combined heat and power (CHP) project profiles, which are available as Adobe Acrobat PDFs.

  1. Midwest Region Combined Heat and Power Projects

    Broader source: Energy.gov [DOE]

    DOE's CHP Technical Assistance Partnerships (CHP TAPs) have compiled a select number of combined heat and power (CHP) project profiles, which are available as Adobe Acrobat PDFs. 

  2. Northwest Region Combined Heat and Power Projects

    Broader source: Energy.gov [DOE]

    DOE's Regional CHP Technical Assistance Partnerships (CHP TAPs) have compiled a select number of combined heat and power (CHP) project profiles, which are available as Adobe Acrobat PDFs.

  3. Pacific Region Combined Heat and Power Projects

    Broader source: Energy.gov [DOE]

    DOE's Regional CHP Technical Assistance Partnerships (CHP TAPs) have compiled a select number of combined heat and power (CHP) project profiles, which are available as Adobe Acrobat PDFs.

  4. V-215: NetworkMiner Directory Traversal and Insecure Library...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    IMPACT: System access SOLUTION: Update to version 1.5. Addthis Related Articles U-198: IBM Lotus Expeditor Multiple Vulnerabilities U-146: Adobe ReaderAcrobat Multiple...

  5. Northeast Region Combined Heat and Power Projects

    Office of Energy Efficiency and Renewable Energy (EERE)

    DOE's Regional CHP Technical Assistance Partnerships (CHP TAPs) have compiled a select number of combined heat and power (CHP) project profiles, which are available as Adobe Acrobat PDFs.

  6. ANR @ MSUANR @ MSU AgBioResearchAgBioResearch Expert Search

    E-Print Network [OSTI]

    at the following WEB address: http://www.adobe.com/products/acrobat/readstep2.html Fill out steps one and two

  7. Notice of Privacy Practice for Patients (HIPAA) Your privacy and the confidentiality of your medical information has always been a commitment of Washington

    E-Print Network [OSTI]

    Grant, Gregory

    medical information has always been a commitment of Washington University physicians. Please select from-Jewish Hospital, St. Louis Children's Hospital or Washington University Short form in an Adobe Acrobat Version · Short form for patients of Washington University Short form in an Adobe Acrobat Version · Full

  8. Adobe Photoshop PDF

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 OutreachProductswsicloudwsicloudden DocumentationAccommodationsRegister / Vol.Conference

  9. Get Adobe Reader Now!

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics AndBeryllium Disease | Department of Energy FormerGE-Prolec CCEGaryGeothermal Energy:

  10. Get Adobe Reader Now!

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration would likeUniverse (Journalvivo Low-Dose Low LETUseful Links Useful Links: TheGerard*3883!Get

  11. Get Adobe Reader Now!

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration would likeUniverse (Journalvivo Low-Dose Low LETUseful Links Useful Links:

  12. This document is available in two formats: this web page (for browsing content) and PDF (comparable to original document formatting). To view the PDF you will need Acrobat Reader, which may be downloaded from the

    E-Print Network [OSTI]

    Shamos, Michael I.

    does not constitute any admission by any party regarding any issue of fact or law; AND WHEREAS or participation with any of them who shall have received actual notice of this UNITED STATES OF AMERICA, Plaintiff is or is contemplating: 1. developing, distributing, promoting, using, selling, or licensing any software that competes

  13. Joshua A. Gage 3250 Sourdough Road 4065701060 Bozeman, Montana 59715 joshgage@gmail.com

    E-Print Network [OSTI]

    Whitlock, Cathy L.

    , Montana Paleoecology Lab Manager · Conducted different aspects of paleoecological research of paleoecological data · Developed webpage for lab using Siteseer program · Handled administrative tasks in lab.2 · Graphic: Adobe Photoshop, Illustrator and Acrobat · Web Design: Siteseer (www.montana.edu/paleoecology

  14. Waste Minimization- The Challenge of the 90's 

    E-Print Network [OSTI]

    Durham, R.

    1989-01-01

    together in this PDF Package. Adobe recommends using Adobe Reader or Adobe Acrobat version 8 or later to work with documents contained within a PDF Package. By updating to the latest version, you’ll enjoy the following benefits: • Efficient, integrated... PDF viewing • Easy printing • Quick searches Don’t have the latest version of Adobe Reader? Click here to download the latest version of Adobe Reader If you already have Adobe Reader 8, click a file in this PDF Package to view it. ...

  15. P&T Dossier Compilation Best Practices: Read departments Role and Scope. Attend appropriate training.

    E-Print Network [OSTI]

    Maxwell, Bruce D.

    P&T Dossier Compilation Best Practices: Read departments Role and Scope. Attend appropriate. Adobe Acrobat Pro is a good tool to use when compiling your dossier. It has many features to assist the web. 4. When you choose an Option for compiling your dossier, follow it through the entire dossier. 5

  16. THE U.S. CONGRESS THE U.S. SECRETARY OF ENERGY

    E-Print Network [OSTI]

    THE U.S. CONGRESS AND THE U.S. SECRETARY OF ENERGY NUCLEAR WASTE TECHNICAL REVIEW BOARD FROM THE December 1992 SIXTH REPORT TO #12;Please Note: The Adobe Acrobat version of this NWTRB report was produced using different publishing software than was used during original report production. Therefore, this pdf

  17. THE U.S. CONGRESS THE U.S. SECRETARY OF ENERGY

    E-Print Network [OSTI]

    THE U.S. CONGRESS AND THE U.S. SECRETARY OF ENERGY NUCLEAR WASTE TECHNICAL REVIEW BOARD FROM THE December 1991 FOURTH REPORT TO #12;Please Note: The Adobe Acrobat version of this NWTRB report was produced using different publishing software than was used during original report production. Therefore, this pdf

  18. THE U.S. CONGRESS THE U.S. SECRETARY OF ENERGY

    E-Print Network [OSTI]

    THE U.S. CONGRESS AND THE U.S. SECRETARY OF ENERGY NUCLEAR WASTE TECHNICAL REVIEW BOARD FROM THE June 1992 FIFTH REPORT TO #12;Please Note: The Adobe Acrobat version of this NWTRB report was produced using different publishing software than was used during original report production. Therefore, this pdf

  19. Annual Report and Accounts

    E-Print Network [OSTI]

    to download now: www.adobe.co.uk/products/acrobat/readstep2.html The PDF has a simple navigation, which Forestry Strategy 15 Sustainable forestry 20 Sustainable economic growth 25 Health & well-being 32 Natural and Groups Selected Extracts from Speeches and Press Releases Grants and Licences ­ Applicants' Charter

  20. V-087: Adobe Flash Player Two Vulnerabilities

    Broader source: Energy.gov [DOE]

    Two vulnerabilities are reported as 0-day which can be exploited by malicious people to compromise a user's system.

  1. Acrobat PDFMaker 5.0 | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i n c i p a l De p u t y A s sconveyance(EPACT) 1EmergencyGJuneSubject:

  2. Water Formatics Engineered formation of nanobubbles networks

    E-Print Network [OSTI]

    Jacob, Eshel Ben

    Water Formatics Engineered formation of nanobubbles networks in water and aqueous solutions We present the idea that the anomalous effects of rf-treatments of water and aqueous solution resulted from-bubble exchange interactions. These exchange interactions are mediated by the ordering of the water molecules

  3. Planet formation and migration

    E-Print Network [OSTI]

    John C B Papaloizou; Caroline Terquem

    2005-11-28

    We review the observations of extrasolar planets, ongoing developments in theories of planet formation, orbital migration, and the evolution of multiplanet systems.

  4. Notes on Star Formation

    E-Print Network [OSTI]

    Krumholz, Mark R

    2015-01-01

    This book provides an introduction to the field of star formation at a level suitable for graduate students or advanced undergraduates in astronomy or physics. The structure of the book is as follows. The first two chapters begin with a discussion of observational techniques, and the basic phenomenology they reveal. The goal is to familiarize students with the basic techniques that will be used throughout, and to provide a common vocabulary for the rest of the book. The next five chapters provide a similar review of the basic physical processes that are important for star formation. Again, the goal is to provide a basis for what follows. The remaining chapters discuss star formation over a variety of scales, starting with the galactic scale and working down to the scales of individual stars and their disks. The book concludes with a brief discussion of the clearing of disks and the transition to planet formation. The book includes five problem sets, complete with solutions.

  5. Word formation in Thadou

    E-Print Network [OSTI]

    Haokip, Pauthang

    2014-01-01

    As stated above, compound words of Thadou are mostlyNote that the resulting new words are always nouns. a. b. c.bad’ (negative) Haokip: Word formation in Thadou a. â-sâa ?

  6. NEWS & VIEWS PATTERN FORMATION

    E-Print Network [OSTI]

    Loss, Daniel

    no apologies for investing energy into problems of specific application to a particular process in nature, and having the curiosity to want to find out how they work. The general public, and especially children flow/surface growth system in a rarely explored region of parameter space for such pattern formation

  7. Isolating Triggered Star Formation

    E-Print Network [OSTI]

    Elizabeth J. Barton; Jacob A. Arnold; Andrew R. Zentner; James S. Bullock; Risa H. Wechsler

    2007-08-21

    Galaxy pairs provide a potentially powerful means of studying triggered star formation from galaxy interactions. We use a large cosmological N-body simulation coupled with a well-tested semi-analytic substructure model to demonstrate that the majority of galaxies in close pairs reside within cluster or group-size halos and therefore represent a biased population, poorly suited for direct comparison to ``field'' galaxies. Thus, the frequent observation that some types of galaxies in pairs have redder colors than ``field'' galaxies is primarily a selection effect. We select galaxy pairs that are isolated in their dark matter halos with respect to other massive subhalos (N=2 halos) and a control sample of isolated galaxies (N=1 halos) for comparison. We then apply these selection criteria to a volume-limited subset of the 2dF Galaxy Redshift Survey with M_Bj ~ 5 above their average past value, while only 10% of isolated galaxies in the control sample show this level of enhancement. Thus, 14% (20 %) of the galaxies in these close pairs show clear triggered star formation. The isolation criteria we develop provide a means to constrain star formation and feedback prescriptions in hydrodynamic simulations and a very general method of understanding the importance of triggered star formation in a cosmological context. (Abridged.)

  8. Emptiness Formation Probability

    E-Print Network [OSTI]

    Nicholas Crawford; Stephen Ng; Shannon Starr

    2014-12-30

    We present rigorous upper and lower bounds on the emptiness formation probability for the ground state of a spin-$1/2$ Heisenberg XXZ quantum spin system. For a $d$-dimensional system we find a rate of decay of the order $\\exp(-c L^{d+1})$ where $L$ is the sidelength of the box in which we ask for the emptiness formation event to occur. In the $d=1$ case this confirms previous predictions made in the integrable systems community, though our bounds do not achieve the precision predicted by Bethe ansatz calculations. On the other hand, our bounds in the case $d \\geq 2$ are new. The main tools we use are reflection positivity and a rigorous path integral expansion which is a variation on those previously introduced by Toth, Aizenman-Nachtergaele and Ueltschi.

  9. U-002:Adobe Photoshop Elements Multiple Memory Corruption Vulnerabilities

    Broader source: Energy.gov [DOE]

    A remote user can create a file that, when loaded by the target user, will execute arbitrary code on the target user's system.

  10. V-131: Adobe Shockwave Player Multiple Vulnerabilities | Department of

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics And Statistics » USAJobs Search USAJobs SearchWater-Savingof Energy

  11. U-035: Adobe Flash Player Multiple Vulnerabilities | Department of Energy

    Office of Environmental Management (EM)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann Jackson About1996HowFOAShowing YouNeed forUnruhDepartment ofM I C H AReactionDepartment35:

  12. Formate-assisted pyrolysis

    DOE Patents [OSTI]

    DeSisto, William Joseph; Wheeler, Marshall Clayton; van Heiningen, Adriaan R. P.

    2015-03-17

    The present invention provides, among other thing, methods for creating significantly deoxygenated bio-oils form biomass including the steps of providing a feedstock, associating the feedstock with an alkali formate to form a treated feedstock, dewatering the treated feedstock, heating the dewatered treated feedstock to form a vapor product, and condensing the vapor product to form a pyrolysis oil, wherein the pyrolysis oil contains less than 30% oxygen by weight.

  13. Petroleum Engineering 321 Formation Evaluation

    E-Print Network [OSTI]

    measurements to estimate hydrocarbon reserves and petrophysical properties of the formation such as porosity Description: Introduction to well-log interpretation for formation evaluation of hydrocarbon, net pay thickness, water/hydrocarbon saturation, permeability, and saturation-dependent capillary

  14. DUST FORMATION IN MACRONOVAE

    SciTech Connect (OSTI)

    Takami, Hajime; Ioka, Kunihito [Institute of Particle and Nuclear Studies, KEK, 1-1, Oho, Tsukuba 305-0801 (Japan); Nozawa, Takaya, E-mail: takami@post.kek.jp, E-mail: kunihito.ioka@kek.jp, E-mail: takaya.nozawa@nao.ac.jp [National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588 (Japan)

    2014-07-01

    We examine dust formation in macronovae (as known as kilonovae), which are the bright ejecta of neutron star binary mergers and one of the leading sites of r-process nucleosynthesis. In light of information about the first macronova candidate associated with GRB 130603B, we find that dust grains of r-process elements have difficulty forming because of the low number density of the r-process atoms, while carbon or elements lighter than iron can condense into dust if they are abundant. Dust grains absorb emission from ejecta with an opacity even greater than that of the r-process elements, and re-emit photons at infrared wavelengths. Such dust emission can potentially account for macronovae without r-process nucleosynthesis as an alternative model. This dust scenario predicts a spectrum with fewer features than the r-process model and day-scale optical-to-ultraviolet emission.

  15. Treating tar sands formations with karsted zones

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Karanikas, John Michael (Houston, TX)

    2010-03-09

    Methods for treating a tar sands formation are described herein. The tar sands formation may have one or more karsted zones. Methods may include providing heat from one or more heaters to one or more karsted zones of the tar sands formation to mobilize fluids in the formation. At least some of the mobilized fluids may be produced from the formation.

  16. Use-driven concept formation

    E-Print Network [OSTI]

    Roberts, Jennifer M. (Jennifer Marie)

    2010-01-01

    When faced with a complex task, humans often identify domain-specific concepts that make the task more tractable. In this thesis, I investigate the formation of domain-specific concepts of this sort. I propose a set of ...

  17. Brown dwarf formation Gilles Chabrier

    E-Print Network [OSTI]

    Joergens, Viki

    : not observed ! Constraints on BD formation/ejection by disk instability: magnetic field No B (pure hydro accretion - Collapse of a cloud -> starts forming small N-body clusters of small (~10-3 Msol

  18. Cross Domain Mathematical Concept Formation 

    E-Print Network [OSTI]

    Steel, Graham; Colton, Simon; Bundy, Alan; Walsh, Toby

    2000-01-01

    Many interesting concepts in mathematics are essentially "cross-domain" in nature, relating objects from more than one area of mathematics, e.g. prime order groups. These concepts are often vital to the formation of a ...

  19. SW New Mexico Oil Well Formation Tops

    SciTech Connect (OSTI)

    Shari Kelley

    2015-10-21

    Rock formation top picks from oil wells from southwestern New Mexico from scout cards and other sources. There are differing formation tops interpretations for some wells, so for those wells duplicate formation top data are presented in this file.

  20. Organic Tandem Solar Cells: Design and Formation

    E-Print Network [OSTI]

    Chen, Chun-Chao

    2015-01-01

    Angeles Organic Tandem Solar Cells: Design and Formation AOrganic Tandem Solar Cells: Design and Formation by Chun-multi-junction tandem solar-cell design. Given this design,

  1. REGULATORY COOPERATION COUNCIL - WORK PLANNING FORMAT: Natural...

    Energy Savers [EERE]

    FORMAT: Natural Gas Use in Transportation REGULATORY COOPERATION COUNCIL - WORK PLANNING FORMAT: Natural Gas Use in Transportation RCC Workplan NGV.PDF More Documents &...

  2. Texas Rice, Volume IV, Number 4 

    E-Print Network [OSTI]

    2004-01-01

    to double check something you had read? How often have you tried to do this and then given up and instead resumed your reading where you left off? Downloaded pdf articles can be searched di- rectly from your computer, using software such as Adobe Acrobat... that you download from the internet can lit- erally last for ever, and as notebook computers become less and less expensive and as the quality of their screens continue to improve, you can increasingly use them in more places around the house or yard...

  3. Formation of porous gas hydrates

    E-Print Network [OSTI]

    Salamatin, Andrey N

    2015-01-01

    Gas hydrates grown at gas-ice interfaces are examined by electron microscopy and found to have a submicron porous texture. Permeability of the intervening hydrate layers provides the connection between the two counterparts (gas and water molecules) of the clathration reaction and makes further hydrate formation possible. The study is focused on phenomenological description of principal stages and rate-limiting processes that control the kinetics of the porous gas hydrate crystal growth from ice powders. Although the detailed physical mechanisms involved in the porous hydrate formation still are not fully understood, the initial stage of hydrate film spreading over the ice surface should be distinguished from the subsequent stage which is presumably limited by the clathration reaction at the ice-hydrate interface and develops after the ice grain coating is finished. The model reveals a time dependence of the reaction degree essentially different from that when the rate-limiting step of the hydrate formation at...

  4. UTS: Library Downloading an eBook into

    E-Print Network [OSTI]

    University of Technology, Sydney

    and install the Mac or PC version on your computer. Please note the public computers in the Library do on public library computers. 3- Select the loan length and select the format desired if the optionUTS: Library Downloading an eBook into Adobe Digital Editions February 2015 #12;Adobe Digital

  5. FED, the Font "EDitor" and Font Formats

    E-Print Network [OSTI]

    Cohen, Joseph D.

    This memo describes FED, a program used for compiling and inspecting fonts: AST font format, a text format which can be used to create and edit fonts: and KST font format, the binary format used by SCRIMP, TJ6, and PUB.

  6. Method of fracturing a geological formation

    DOE Patents [OSTI]

    Johnson, James O. (2679-B Walnut, Los Alamos, NM 87544)

    1990-01-01

    An improved method of fracturing a geological formation surrounding a well bore is disclosed. A relatively small explosive charge is emplaced in a well bore and the bore is subsequently hydraulically pressurized to a pressure less than the formation breakdown pressure and preferably greater than the fracture propagation pressure of the formation. The charge is denoted while the bore is so pressurized, resulting in the formation of multiple fractures in the surrounding formation with little or no accompanying formation damage. Subsequent hydraulic pressurization can be used to propagate and extend the fractures in a conventional manner. The method is useful for stimulating production of oil, gas and possibly water from suitable geologic formations.

  7. The Epoch of Galaxy Formation

    E-Print Network [OSTI]

    Raul Jimenez

    2001-10-09

    I present a biased review of when the epoch of formation of galaxies (both disks and ellipticals) maybe took place. I base my arguments in simple (mostly) analytic models that have been recently developed to reproduce most of the observed photometric, chemical and dynamical properties of galaxies both at low and high redshift.

  8. Earth and Terrestrial Planet Formation

    E-Print Network [OSTI]

    Jacobson, Seth A

    2015-01-01

    The growth and composition of Earth is a direct consequence of planet formation throughout the Solar System. We discuss the known history of the Solar System, the proposed stages of growth and how the early stages of planet formation may be dominated by pebble growth processes. Pebbles are small bodies whose strong interactions with the nebula gas lead to remarkable new accretion mechanisms for the formation of planetesimals and the growth of planetary embryos. Many of the popular models for the later stages of planet formation are presented. The classical models with the giant planets on fixed orbits are not consistent with the known history of the Solar System, fail to create a high Earth/Mars mass ratio, and, in many cases, are also internally inconsistent. The successful Grand Tack model creates a small Mars, a wet Earth, a realistic asteroid belt and the mass-orbit structure of the terrestrial planets. In the Grand Tack scenario, growth curves for Earth most closely match a Weibull model. The feeding zon...

  9. Cloud Formation, Evolution and Destruction

    E-Print Network [OSTI]

    Estalella, Robert

    Chapter 4 Cloud Formation, Evolution and Destruction We now begin to trace the journey towards a star. How long does this take? The answer is surprisingly short: a good many clouds already contain new stars and these stars tend to be young. The typical cloud cannot spend long, if any time at all

  10. Treating tar sands formations with dolomite

    DOE Patents [OSTI]

    Vinegar, Harold J.; Karanikas, John Michael

    2010-06-08

    Methods for treating a tar sands formation are described herein. The tar sands formation may include dolomite and hydrocarbons. Methods may include providing heat at less than the decomposition temperature of dolomite from one or more heaters to at least a portion of the formation. At least some of the hydrocarbon fluids are mobilized in the formation. At least some of the hydrocarbon fluids may be produced from the formation.

  11. Rapid gas hydrate formation process

    DOE Patents [OSTI]

    Brown, Thomas D.; Taylor, Charles E.; Unione, Alfred J.

    2013-01-15

    The disclosure provides a method and apparatus for forming gas hydrates from a two-phase mixture of water and a hydrate forming gas. The two-phase mixture is created in a mixing zone which may be wholly included within the body of a spray nozzle. The two-phase mixture is subsequently sprayed into a reaction zone, where the reaction zone is under pressure and temperature conditions suitable for formation of the gas hydrate. The reaction zone pressure is less than the mixing zone pressure so that expansion of the hydrate-forming gas in the mixture provides a degree of cooling by the Joule-Thompson effect and provides more intimate mixing between the water and the hydrate-forming gas. The result of the process is the formation of gas hydrates continuously and with a greatly reduced induction time. An apparatus for conduct of the method is further provided.

  12. Controlled Irradiative Formation of Penitentes

    E-Print Network [OSTI]

    V. Bergeron; C. Berger; M. D. Betterton

    2006-01-24

    Spike-shaped structures are produced by light-driven ablation in very different contexts. Penitentes 1-4 m high are common on Andean glaciers, where their formation changes glacier dynamics and hydrology. Laser ablation can produce cones 10-100 microns high with a variety of proposed applications in materials science. We report the first laboratory generation of centimeter-scale snow and ice penitentes. Systematically varying conditions allows identification of the essential parameters controlling the formation of ablation structures. We demonstrate that penitente initiation and coarsening requires cold temperatures, so that ablation leads to sublimation rather than melting. Once penitentes have formed, further growth of height can occur by melting. The penitentes intially appear as small structures (3 mm high) and grow by coarsening to 1-5 cm high. Our results are an important step towards understanding and controlling ablation morphologies.

  13. Laser beam pulse formatting method

    DOE Patents [OSTI]

    Daly, T.P.; Moses, E.I.; Patterson, R.W.; Sawicki, R.H.

    1994-08-09

    A method for formatting a laser beam pulse using one or more delay loops is disclosed. The delay loops have a partially reflective beam splitter and a plurality of highly reflective mirrors arranged such that the laser beam pulse enters into the delay loop through the beam splitter and circulates therein along a delay loop length defined by the mirrors. As the laser beam pulse circulates within the delay loop a portion thereof is emitted upon each completed circuit when the laser beam pulse strikes the beam splitter. The laser beam pulse is thereby formatted into a plurality of sub-pulses. The delay loops are used in combination to produce complex waveforms by combining the sub-pulses using additive waveform synthesis. 8 figs.

  14. Shock Formation in Lovelock Theories

    E-Print Network [OSTI]

    Harvey S. Reall; Norihiro Tanahashi; Benson Way

    2014-09-12

    We argue that Lovelock theories of gravity suffer from shock formation, unlike General Relativity. We consider the propagation of (i) a discontinuity in curvature, and (ii) weak, high frequency, gravitational waves. Such disturbances propagate along characteristic hypersurfaces of a "background" spacetime and their amplitude is governed by a transport equation. In GR the transport equation is linear. In Lovelock theories, it is nonlinear and its solutions can blow up, corresponding to the formation of a shock. We show that this effect is absent in some simple cases e.g. a flat background spacetime, and demonstrate its presence for a plane wave background. We comment on weak cosmic censorship, the evolution of shocks, and the nonlinear stability of Minkowski spacetime, in Lovelock theories.

  15. Membrane adhesion and domain formation

    E-Print Network [OSTI]

    Thomas R. Weikl; Reinhard Lipowsky

    2007-09-23

    We review theoretical results for the adhesion-induced phase behavior of biomembranes. The focus is on models in which the membranes are represented as discretized elastic sheets with embedded adhesion molecules. We present several mechanism that lead to the formation of domains during adhesion, and discuss the time-dependent evolution of domain patterns obtained in Monte-Carlo simulations. The simulated pattern dynamics has striking similarities to the pattern evolution observed during T cell adhesion.

  16. Absorption and elimination of formate following oral administration of calcium formate in female human subjects

    E-Print Network [OSTI]

    Hanzlik, Robert P.; Fowler, Stephen C.; Eells, Janis T.

    2005-02-01

    Published abstract: Calcium formate is a water-soluble salt of an essential mineral nutrient with potential for use as a dietary calcium supplement. Formate ion is a product of endogenous and xenobiotic metabolism, but sustained high plasma formate...

  17. Structure formation: Models, Dynamics and Status

    E-Print Network [OSTI]

    T. Padmanabhan

    1995-08-25

    The constraints on the models for the structure formation arising from various cosmological observations at different length scales are reviewed. The status of different models for structure formation is examined critically in the light of these observations.

  18. XML Format for SESAME and LEOS

    SciTech Connect (OSTI)

    Durrenberger, J K; Neely, J R; Sterne, P A

    2009-04-29

    The objective of this document is to describe the XML format used by LLNL and LANL to represent the equation-of-state and related material information in the LEOS and SESAME data libraries. The primary purpose of this document is to describe a specific XML format for representing EOS data that is tailored to the nature of the underlying data and is amenable to conversion to both legacy SESAME and LEOS binary formats. The secondary purpose is to describe an XML format that lends itself to a 'natural' representation in a binary file format of the SESAME, pdb or hdf5 form so that this format and related tools can be used for the rapid and efficient development and implementation of prototype data structures. This document describes the XML format only. A working knowledge of LEOS and SESAME formats is assumed.

  19. Dynamics and control of electromagnetic satellite formations

    E-Print Network [OSTI]

    Ahsun, Umair, 1972-

    2007-01-01

    Satellite formation flying is an enabling technology for many space missions, especially for space-based telescopes. Usually there is a tight formation-keeping requirement that may need constant expenditure of fuel or at ...

  20. Formation damage in underbalanced drilling operations 

    E-Print Network [OSTI]

    Reyes Serpa, Carlos Alberto

    2003-01-01

    Formation damage has long been recognized as a potential source of reduced productivity and injectivity in both horizontal and vertical wells. From the moment that the pay zone is being drilled until the well is put on production, a formation...

  1. La cl informatique Formation Word XP

    E-Print Network [OSTI]

    Vellend, Mark

    La clé informatique Formation Word XP Aide-mémoire Hiver 2004 #12;#12;Formation Word XP Hiver 2004 1. PRÉSENTATION DE L'INTERFACE DE MICROSOFT WORD XP................ 1 1.1. L'interface générale

  2. Proportional structural effects of formative indicators

    E-Print Network [OSTI]

    Franke, George R.; Preacher, Kristopher J.; Rigdon, Ed E.

    2009-03-15

    that are proportional to their effects on the formative construct itself. This constraint has important implications for developing and testing formative models. This study demonstrates the existence of the constraint, shows that researchers must consider...

  3. Treating nahcolite containing formations and saline zones

    DOE Patents [OSTI]

    Vinegar, Harold J

    2013-06-11

    A method for treating a nahcolite containing subsurface formation includes removing water from a saline zone in or near the formation. The removed water is heated using a steam and electricity cogeneration facility. The heated water is provided to the nahcolite containing formation. A fluid is produced from the nahcolite containing formation. The fluid includes at least some dissolved nahcolite. At least some of the fluid is provided to the saline zone.

  4. Electromagnetic Formation Flight of Satellite Arrays

    E-Print Network [OSTI]

    Electromagnetic Formation Flight of Satellite Arrays Daniel W. Kwon and David W. Miller February 2005 SSL # 2-05 #12;#12;Electromagnetic Formation Flight of Satellite Arrays By DANIEL W. KWON S;#12;Electromagnetic Formation Flight of Satellite Arrays by DANIEL W. KWON Submitted to the Department of Aeronautics

  5. Electrochemical formation of field emitters

    SciTech Connect (OSTI)

    Bernhardt, Anthony F. (Berkeley, CA)

    1999-01-01

    Electrochemical formation of field emitters, particularly useful in the fabrication of flat panel displays. The fabrication involves field emitting points in a gated field emitter structure. Metal field emitters are formed by electroplating and the shape of the formed emitter is controlled by the potential imposed on the gate as well as on a separate counter electrode. This allows sharp emitters to be formed in a more inexpensive and manufacturable process than vacuum deposition processes used at present. The fabrication process involves etching of the gate metal and the dielectric layer down to the resistor layer, and then electroplating the etched area and forming an electroplated emitter point in the etched area.

  6. Petrophysical evaluation of subterranean formations

    DOE Patents [OSTI]

    Klein, James D; Schoderbek, David A; Mailloux, Jason M

    2013-05-28

    Methods and systems are provided for evaluating petrophysical properties of subterranean formations and comprehensively evaluating hydrate presence through a combination of computer-implemented log modeling and analysis. Certain embodiments include the steps of running a number of logging tools in a wellbore to obtain a variety of wellbore data and logs, and evaluating and modeling the log data to ascertain various petrophysical properties. Examples of suitable logging techniques that may be used in combination with the present invention include, but are not limited to, sonic logs, electrical resistivity logs, gamma ray logs, neutron porosity logs, density logs, NRM logs, or any combination or subset thereof.

  7. Formation Flying and Deformable Instruments

    SciTech Connect (OSTI)

    Rio, Yvon

    2009-05-11

    Astronomers have always attempted to build very stable instruments. They fight all that can cause mechanical deformation or image motion. This has led to well established technologies (autoguide, active optics, thermal control, tip/tilt correction), as well as observing methods based on the use of controlled motion (scanning, micro scanning, shift and add, chopping and nodding). Formation flying disturbs this practice. It is neither possible to reduce the relative motion to very small amplitudes, nor to control it at will. Some impacts on Simbol-X instrument design, and operation are presented.

  8. Heating tar sands formations while controlling pressure

    DOE Patents [OSTI]

    Stegemeier, George Leo (Houston, TX) [Houston, TX; Beer, Gary Lee (Houston, TX) [Houston, TX; Zhang, Etuan (Houston, TX) [Houston, TX

    2010-01-12

    Methods for treating a tar sands formation are described herein. Methods may include heating at least a section of a hydrocarbon layer in the formation from a plurality of heaters located in the formation. A pressure in the majority of the section may be maintained below a fracture pressure of the formation. The pressure in the majority of the section may be reduced to a selected pressure after the average temperature reaches a temperature that is above 240.degree. C. and is at or below pyrolysis temperatures of hydrocarbons in the section. At least some hydrocarbon fluids may be produced from the formation.

  9. Coring in deep hardrock formations

    SciTech Connect (OSTI)

    Drumheller, D.S.

    1988-08-01

    The United States Department of Energy is involved in a variety of scientific and engineering feasibility studies requiring extensive drilling in hard crystalline rock. In many cases well depths extend from 6000 to 20,000 feet in high-temperature, granitic formations. Examples of such projects are the Hot Dry Rock well system at Fenton Hill, New Mexico and the planned exploratory magma well near Mammoth Lakes, California. In addition to these programs, there is also continuing interest in supporting programs to reduce drilling costs associated with the production of geothermal energy from underground sources such as the Geysers area near San Francisco, California. The overall progression in these efforts is to drill deeper holes in higher temperature, harder formations. In conjunction with this trend is a desire to improve the capability to recover geological information. Spot coring and continuous coring are important elements in this effort. It is the purpose of this report to examine the current methods used to obtain core from deep wells and to suggest projects which will improve existing capabilities. 28 refs., 8 figs., 2 tabs.

  10. Coke formation in visbreaking process

    SciTech Connect (OSTI)

    Yan, T.Y. )

    1987-04-01

    Visbreaking is a mild cracking process primarily used to reduce residual oil viscosity and thus decrease the amount of cutter stock required for blending to heavy fuels specification. It can also be used to produce incremental quantities of gasoline, middle distillates and catalytic cracker feeds. This process was widely used in the 1930s and 1940s and became obsolete until a few years ago. When the need for increased conversion of residues to light products became desirable, visbreaking offered economic advantages to many refining schemes - especially in Western Europe. Between 1978-1981, Exxon brought on stream seven visbreakers ranging from 1900 to 9100 tons/SD capacity. In January 1983, the world-wide visbreaking capacity was over 2 MM B/SD. The visbreaking process and its application in refinery operations have been well described. In general, the process economics improve as the process severity is increased but it is limited by coke formation in the process. For this reason, they have studied the kinetics of coke formation in the visbreaking process.

  11. Electrochemical formation of field emitters

    DOE Patents [OSTI]

    Bernhardt, A.F.

    1999-03-16

    Electrochemical formation of field emitters, particularly useful in the fabrication of flat panel displays is disclosed. The fabrication involves field emitting points in a gated field emitter structure. Metal field emitters are formed by electroplating and the shape of the formed emitter is controlled by the potential imposed on the gate as well as on a separate counter electrode. This allows sharp emitters to be formed in a more inexpensive and manufacturable process than vacuum deposition processes used at present. The fabrication process involves etching of the gate metal and the dielectric layer down to the resistor layer, and then electroplating the etched area and forming an electroplated emitter point in the etched area. 12 figs.

  12. Adaptive Optics in Star Formation

    E-Print Network [OSTI]

    Wolfgang Brandner

    2003-09-29

    Over the past ten years, the concept of adaptive optics has evolved from early experimental stages to a standard observing tool now available at almost all major optical and near-infrared telescope facilities. Adaptive optics will also be essential in exploiting the full potential of the large optical/infrared interferometers currently under construction. Both observations with high-angular resolution and at high contrast, and with a high point source sensitivity are facilitated by adaptive optics. Among the areas which benefit most from the use of adaptive optics are studies of the circumstellar environment (envelopes, disks, outflows), substellar companions and multiple systems, and dense young stellar populations. This contribution highlights some of the recent advances in star formation studies facilitated by adaptive optics, and gives a brief tutorial on optimized observing and data reduction strategies.

  13. Formation of helical ion chains

    E-Print Network [OSTI]

    Ramil Nigmatullin; Adolfo del Campo; Gabriele De Chiara; Giovanna Morigi; Martin B. Plenio; Alex Retzker

    2015-08-25

    We study the nonequilibrium dynamics of the linear to zigzag structural phase transition exhibited by an ion chain confined in a trap with periodic boundary conditions. The transition is driven by reducing the transverse confinement at a finite quench rate, which can be accurately controlled. This results in the formation of zigzag domains oriented along different transverse planes. The twists between different domains can be stabilized by the topology of the trap and under laser cooling the system has a chance to relax to a helical chain with nonzero winding number. Molecular dynamics simulations are used to obtain a large sample of possible trajectories for different quench rates. The scaling of the average winding number with different quench rates is compared to the prediction of the Kibble-Zurek theory, and a good quantitative agreement is found.

  14. Methanol Masers and Star Formation

    E-Print Network [OSTI]

    A. M. Sobolev; A. B. Ostrovskii; M. S. Kirsanova; O. V. Shelemei; M. A. Voronkov; A. V. Malyshev

    2006-01-12

    Methanol masers which are traditionally divided into two classes provide possibility to study important parts of the star forming regions: Class~II masers trace vicinities of the massive YSOs while class~I masers are likely to trace more distant parts of the outflows where newer stars can form. There are many methanol transitions which produce observed masers. This allows to use pumping analysis for estimation of the physical parameters in the maser formation regions and its environment, for the study of their evolution. Extensive surveys in different masing transitions allow to conclude on the values of the temperatures, densities, dust properties, etc. in the bulk of masing regions. Variability of the brightest masers is monitored during several years. In some cases it is probably caused by the changes of the dust temperature which follow variations in the brightness of the central YSO reflecting the character of the accretion process. A unified catalogue of the class II methanol masers consisting of more than 500 objects is compiled. Analysis of the data shows that: physical conditions within the usual maser source vary considerably; maser brightness is determined by parameters of some distinguished part of the object - maser formation region; class II methanol masers are formed not within the outflows but in the regions affected by their propagation. It is shown that the "near" solutions for the kinematic distances to the sources can be used for statistical analysis. The luminosity function of the 6.7 GHz methanol masers is constructed. It is shown that improvement of the sensitivity of surveys can increase number of detected maser sources considerably.

  15. Radio Triggered Star Formation in Cooling Flows

    E-Print Network [OSTI]

    B. R. McNamara

    1999-11-08

    The giant galaxies located at the centers of cluster cooling flows are frequently sites of vigorous star formation. In some instances, star formation appears to have been triggered by the galaxy's radio source. The colors and spectral indices of the young populations are generally consistent with short duration bursts or continuous star formation for durations much less than 1 Gyr, which is less than the presumed ages of cooling flows. The star formation properties are inconsistent with fueling by a continuously accreting cooling flow, although the prevalence of star formation is consistent with repeated bursts and periodic refueling. Star formation may be fueled, in some cases, by cold material stripped from neighboring cluster galaxies.

  16. Floating insulated conductors for heating subsurface formations

    DOE Patents [OSTI]

    Burns, David; Goodwin, Charles R.

    2014-07-29

    A heating system for a subsurface formation includes a conduit located in a first opening in the subsurface formation. Three electrical conductors are located in the conduit. A return conductor is located inside the conduit. The return conductor is electrically coupled to the ends of the electrical conductors distal from the surface of the formation. Insulation is located inside the conduit. The insulation electrically insulates the three electrical conductors, the return conductor, and the conduit from each other.

  17. Heating systems for heating subsurface formations

    DOE Patents [OSTI]

    Nguyen, Scott Vinh (Houston, TX); Vinegar, Harold J. (Bellaire, TX)

    2011-04-26

    Methods and systems for heating a subsurface formation are described herein. A heating system for a subsurface formation includes a sealed conduit positioned in an opening in the formation and a heat source. The sealed conduit includes a heat transfer fluid. The heat source provides heat to a portion of the sealed conduit to change phase of the heat transfer fluid from a liquid to a vapor. The vapor in the sealed conduit rises in the sealed conduit, condenses to transfer heat to the formation and returns to the conduit portion as a liquid.

  18. Treating tar sands formations with dolomite

    DOE Patents [OSTI]

    Vinegar, Harold J.; Karanikas, John Michael

    2013-10-15

    A method for treating a karsted formation containing heavy hydrocarbons and dolomite includes providing heat to at least part of one or more karsted layers in the formation from one or more heaters located in the karsted layers. A temperature in at least one of the karsted layers is allowed to reach a decomposition temperature of dolomite in the formation. The dolomite is allowed to decompose and at least some hydrocarbons are produced from at least one of the karsted layers of the formation.

  19. New Particle Formation Study Final Campaign Report

    SciTech Connect (OSTI)

    Smith, JN; McMurry, PH

    2015-01-01

    The scientific foci of the New Particle Formation Study were the formation and evolution of atmospheric aerosols and the impacts of newly formed particles on cloud processes. Specifically, we planned to: (1) to identify the species and mechanisms responsible for the initial steps of new particle formation, i.e., the formation of thermodynamically stable clusters; (2) investigate the role of acid-base chemistry in new particle growth through measurements of ammonia and amines as well as organic and inorganic acids in both atmospheric nanoparticles and the gas phase; (3) investigate the contribution of other surface area or volume-controlled processes to nanoparticle formation and growth; (4) create a comprehensive dataset related to new particle formation and growth that can be used as input for our own thermodynamic models as well as the modeling efforts by our Department of Energy (DOE) Aerosol Life Cycle working group collaborators; (5) characterize the increase of the number and activity of cloud condensation nuclei (CCN) due to particle formation and growth; (6) determine the regional extent of new particle formation to address the role that atmospheric transport plays in determining the impacts, if any, of new particle formation on cloud number and properties.

  20. Hydrogen Adsorption Induces Interlayer Carbon Bond Formation...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Hydrogen Adsorption Induces Interlayer Carbon Bond Formation in Supported Few-Layer Graphene Friday, February 28, 2014 Among the allotropes of carbon, diamond has some of the most...

  1. Heating tar sands formations to visbreaking temperatures

    DOE Patents [OSTI]

    Karanikas, John Michael (Houston, TX); Colmenares, Tulio Rafael (Houston, TX); Zhang, Etuan (Houston, TX); Marino, Marian (Houston, TX); Roes, Augustinus Wilhelmus Maria (Houston, TX); Ryan, Robert Charles (Houston, TX); Beer, Gary Lee (Houston, TX); Dombrowski, Robert James (Houston, TX); Jaiswal, Namit (Houston, TX)

    2009-12-22

    Methods for treating a tar sands formation are described herein. Methods may include heating at least a section of a hydrocarbon layer in the formation from a plurality of heaters located in the formation. The heat may be controlled so that at least a majority of the section reaches an average temperature of between 200.degree. C. and 240.degree. C., which results in visbreaking of at least some hydrocarbons in the section. At least some visbroken hydrocarbon fluids may be produced from the formation.

  2. Standard Format and Content for Emergency Plans

    Broader source: Directives, Delegations, and Requirements [Office of Management (MA)]

    1997-08-21

    This volume addresses recommended emergency plan format and content for Operational Emergency Base Programs and Operational Emergency Hazardous Material Programs. Canceled by DOE G 151.1-3.

  3. Format requirements of thermal neutron scattering data in a nuclear data format to succeed the ENDF format

    SciTech Connect (OSTI)

    Brown, D. [Brookhaven National Lab. (BNL), Upton, NY (United States)

    2014-03-31

    In November 2012, the Working Party on Evaluation Cooperation Subgroup 38 (WPEC-SG38) began with the task of developing a nuclear data format and supporting infrastructure to replace the now nearly 50 year old ENDF format. The first step in this process is to develop requirements for the new format and infrastructure. In this talk, I will review the status of ENDF's Thermal Scattering Law (TSL) formats as well as support for this data in the GND format (from which the new format is expected to evolve). Finally, I hope to begin a dialog with members of the thermal neutron scattering community so that their data needs can be accurately and easily accommodated by the new format and tools, as captured by the requirements document. During this discussion, we must keep in mind that the new tools and format must; Support what is in existing data files; Support new things we want to put in data files; and Be flexible enough for us to adapt it to future unanticipated challenges.

  4. Page 1 of 17 Designate default font for Microsoft Office 2011

    E-Print Network [OSTI]

    Zhou, Chongwu

    The Standard Font selection will default your font settings for all future, new spreadsheets. Select Adobe Caslon Pro from the Font selection in the Standard will need to save the presentation. Save As> Format: Office Theme

  5. Chaos in Terrestrial Planet Formation

    E-Print Network [OSTI]

    Volker Hoffmann; Simon L. Grimm; Ben Moore; Joachim Stadel

    2015-08-04

    Terrestrial planets are thought to be the result of a vast number of gravitational interactions and collisions between smaller bodies. We use numerical simulations to show that practically identical initial conditions result in a wide array of final planetary configurations. This highly chaotic behaviour questions the predictability of different scenarios for the formation and evolution of our solar system and planetary systems in general. However, multiple realisations of the same initial conditions can be used to predict certain global statistics. We present two sets of numerical experiments that quantify this behaviour. Firstly, we demonstrate that simulations with slightly displaced particles are completely divergent after ~500 years, irrespective of initial displacement, particle number, and code accuracy. If a single planetesimal is moved by less than one millimetre, then a different set of planets results -- this timescale for chaotic divergence decreases with increasing particle number. Secondly, we show final planetary configurations of initially similar simulations with and without giant planets after evolving them for ~148 Myr. We find that the same simulations including giant planets tend to generate higher mass planets at lower semi-major axes than simulations without gas giants. This prediction can be tested with forthcoming observational programs. By extracting outliers in the observations, we cautiously predict that Kepler-10, Kepler-9, 61 Vir, HD 134060, and HD 51608 may host as yet undetected giant planets.

  6. Active tails enhance arboreal acrobatics in geckos Ardian Jusufi, Daniel I. Goldman*, Shai Revzen, and Robert J. Full

    E-Print Network [OSTI]

    Goldman, Daniel I.

    behavior, we studied the flat-tailed house gecko, Cosymbotus platyurus, because it is agile and has a sizeable, active tail. Moreover, the dynamics of house geckos' horizontal running (14) and vertical climbing (1) are well characterized. Our results suggest that large tails not only serve as passive

  7. Autonomous Helicopter Formation using Model Predictive Control

    E-Print Network [OSTI]

    Sastry, S. Shankar

    Autonomous Helicopter Formation using Model Predictive Control Hoam Chung and S. Shankar Sastry for teams of helicopters. However, the potential for accidents is greatly increased when helicopter teams to the problem of helicopter formations comprised of heterogenous vehicles. The disturbance attenuation property

  8. FAINT RADIO SOURCES AND STAR FORMATION HISTORY

    E-Print Network [OSTI]

    Waddington, Ian

    FAINT RADIO SOURCES AND STAR FORMATION HISTORY Deborah B. Haarsma 1 , R. Bruce Partridge 1 , Ian 85287­1504 USA Abstract. Faint extragalactic radio sources provide important information about the global history of star formation. Sensitive radio observations of the Hubble Deep Field and other fields

  9. Methods for forming wellbores in heated formations

    DOE Patents [OSTI]

    Guimerans, Rosalvina Ramona; Mansure, Arthur James

    2012-09-25

    A method for forming a wellbore in a heated formation includes flowing liquid cooling fluid to a bottom hole assembly in a wellbore in a heated formation. At least a portion of the liquid cooling fluid is vaporized at or near a region to be cooled. Vaporizing the liquid cooling fluid absorbs heat from the region to be cooled.

  10. Robot Behavior Adaptation for Formation Maintenance

    E-Print Network [OSTI]

    López-Sánchez, Maite

    1 Robot Behavior Adaptation for Formation Maintenance Maite López-Sánchez maite@maia.ub.es WAI): ­1 or 2 reference robots to follow ­keeping fixed angle (formation property) ­and fixed distance d (separation distance) · related to robot visibility range, speed or reaction capabilities Basic behaviors I

  11. First Structure Formation and the First Stars

    E-Print Network [OSTI]

    Michael L. Norman; Tom Abel; Greg Bryan

    2000-05-11

    We discuss the results of recent 3D simulations of first structure formation in relationship to the formation of the first stars. On the basis of a new, high-resolution AMR simulation (spatial dynamic range = 30,000,000), we conclude that the first stars are likely to be massive.

  12. 1.6 Policy Development & Format Page 1 of 3 Policy Development & Format

    E-Print Network [OSTI]

    Hung, I-Kuai

    1.6 Policy Development & Format Page 1 of 3 Policy Development & Format Original Implementation: July 16, 2013 Last Revision: None A. POLICY FORMAT Each policy will have a title that is concise but descriptive. Each policy is indexed with a numeric indicator which indicates the position of the entry within

  13. Sequentially Triggered Star Formation in OB Associations

    E-Print Network [OSTI]

    Thomas Preibisch; Hans Zinnecker

    2006-10-27

    We discuss observational evidence for sequential and triggered star formation in OB associations. We first review the star formation process in the Scorpius-Centaurus OB association, the nearest OB association to the Sun, where several recent extensive studies have allowed us to reconstruct the star formation history in a rather detailed way. We then compare the observational results with those obtained for other OB associations and with recent models of rapid cloud and star formation in the turbulent interstellar medium. We conclude that the formation of whole OB subgroups (each consisting of several thousand stars) requires large-scale triggering mechanisms such as shocks from expanding wind and supernova driven superbubbles surrounding older subgroups. Other triggering mechanisms, like radiatively driven implosion of globules, also operate, but seem to be secondary processes, forming only small stellar groups rather than whole OB subgroups with thousands of stars.

  14. MathNet MathNet Mathematical

    E-Print Network [OSTI]

    de Figueiredo, Luiz Henrique

    Net Types of Data Types of Data . . File formats File formats . . for papers for papers . . html html Distiller) PDF generator (Acrobat Distiller) . . Html (Latex2html) Html (Latex2html) . . Cataloging­Server paradigm Client­Server paradigm . . Distributed Web Servers Distributed Web Servers . . Client:WWW Browser

  15. Star Formation in the Local Milky Way

    E-Print Network [OSTI]

    Lada, Charles J

    2015-01-01

    Studies of molecular clouds and young stars near the sun have provided invaluable insights into the process of star formation. Indeed, much of our physical understanding of this topic has been derived from such studies. Perhaps the two most fundamental problems confronting star formation research today are: 1) determining the origin of stellar mass and 2) deciphering the nature of the physical processes that control the star formation rate in molecular gas. As I will briefly outline here, observations and studies of local star forming regions are making particularly significant contributions toward the solution of both these important problems.

  16. Loop formation in polymers in crowded environment

    E-Print Network [OSTI]

    K. Haydukivska; V. Blavatska

    2015-11-12

    We analyze the probability of a single loop formation in a long flexible polymer chain in disordered environment in $d$ dimensions. The structural defects are considered to be correlated on large distances $r$ according to a power law $\\sim r^{-a}$. Working within the frames of continuous chain model and applying the direct polymer renormalization scheme, we obtain the values of critical exponents governing the scaling of probabilities of loop formation with various positions along the chain as function of loops length. Our results quantitatively reveal that the presence of structural defects in environment decreases the probability of loop formation in polymer macromolecules.

  17. Carbon nanotube formation by laser direct writing

    SciTech Connect (OSTI)

    Wu, Y.-T.; Su, H.-C.; Tsai, C.-M.; Liu, K.-L.; Chen, G.-D.; Huang, R.-H.; Yew, T.-R.

    2008-07-14

    This letter presents carbon nanotube (CNT) formation by laser direct writing using 248 nm KrF excimer pulsed laser in air at room temperature, which was applied to irradiate amorphous carbon (a-C) assisted by Ni catalysts underneath for the transformation of carbon species into CNTs. The CNTs were synthesized under appropriate combination of laser energy density and a-C thickness. The growth mechanism and key parameters to determine the success of CNT formation were also discussed. The demonstration of the CNT growth by laser direct writing in air at room temperature opens an opportunity of in-position CNT formation at low temperatures.

  18. The NeXus data format

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Könnecke, Mark; Akeroyd, Frederick A.; Bernstein, Herbert J.; Brewster, Aaron S.; Campbell, Stuart I.; Clausen, Björn; Cottrell, Stephen; Hoffmann, Jens Uwe; Jemian, Pete R.; Männicke, David; et al

    2015-01-30

    NeXus is an effort by an international group of scientists to define a common data exchange and archival format for neutron, X-ray and muon experiments. NeXus is built on top of the scientific data format HDF5 and adds domain-specific rules for organizing data within HDF5 files, in addition to a dictionary of well defined domain-specific field names. The NeXus data format has two purposes. First, it defines a format that can serve as a container for all relevant data associated with a beamline. This is a very important use case. Second, it defines standards in the form of application definitionsmore »for the exchange of data between applications. NeXus provides structures for raw experimental data as well as for processed data.« less

  19. Mechanisms and Geochemical Models of Core Formation

    E-Print Network [OSTI]

    Rubie, David C

    2015-01-01

    The formation of the Earth's core is a consequence of planetary accretion and processes in the Earth's interior. The mechanical process of planetary differentiation is likely to occur in large, if not global, magma oceans created by the collisions of planetary embryos. Metal-silicate segregation in magma oceans occurs rapidly and efficiently unlike grain scale percolation according to laboratory experiments and calculations. Geochemical models of the core formation process as planetary accretion proceeds are becoming increasingly realistic. Single stage and continuous core formation models have evolved into multi-stage models that are couple to the output of dynamical models of the giant impact phase of planet formation. The models that are most successful in matching the chemical composition of the Earth's mantle, based on experimentally-derived element partition coefficients, show that the temperature and pressure of metal-silicate equilibration must increase as a function of time and mass accreted and so m...

  20. Electromagnetic formation flight dipole solution planning

    E-Print Network [OSTI]

    Schweighart, Samuel A. (Samuel Adam), 1977-

    2005-01-01

    Electromagnetic Formation Flight (EMFF) describes the concept of using electromagnets (coupled with reaction wheels) to provide all of the necessary forces and torques needed to maintain a satellite's relative position and ...

  1. Modeling deposit formation in diesel injector nozzle

    E-Print Network [OSTI]

    Sudhiesh Kumar, Chintoo

    2009-01-01

    Formation of deposit in the diesel injector nozzle affects the injection behavior and hinders performance. Under running condition, deposit precursors are washed away by the ensuing injection. However, during the cool down ...

  2. Electromagnetic formation flight of satellite arrays

    E-Print Network [OSTI]

    Kwon, Daniel W., 1980-

    2005-01-01

    Proposed methods of actuating spacecraft in sparse aperture arrays use propellant as a reaction mass. For formation flying systems, propellant becomes a critical consumable which can be quickly exhausted while maintaining ...

  3. Kinetics of acrylamide formation in potato chips 

    E-Print Network [OSTI]

    Granda, Claudia Esthela

    2006-08-16

    Acrylamide is considered a carcinogen in animals and a possible carcinogen in humans. It has been found in starch rich foods cooked at high temperatures. Vacuum frying (10 Torr) was studied as a possible alternative to reduce acrylamide formation...

  4. HYDROCARBON FORMATION ON POLYMER-SUPPORTED COBALT

    E-Print Network [OSTI]

    Benner, Linda S.

    2013-01-01

    NV~ August 25-29, 1980 HYDROCARBON FORMATION ON POLYMER-catalyzed reduction of CO to hydrocarbons Tropscb. Among theof CO to saturated linear hydrocarbons and appears to retain

  5. Modelling and control of satellite formations 

    E-Print Network [OSTI]

    Vaddi, Veera Venkata Sesha Sai

    2004-09-30

    ®erent satellites in a formation. To achieve the various mission objectives it is necessary for a formation to recon¯gure itself periodically. An analytical impulsive control scheme has been developed for this purpose. This control scheme has the distinct advantage... . . . . . . . . . . . . . . . . . . 15 1.4.2 Impulsive Control . . . . . . . . . . . . . . . . . . . 16 1.5 Goals . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17 1.6 Nonlinearity and Eccentricity Perturbations . . . . . . . . 18 1.7 Linear and Nonlinear Controllers...

  6. Situ microbial plugging process for subterranean formations

    DOE Patents [OSTI]

    McInerney, Michael J. (Norman, OK); Jenneman, Gary E. (Norman, OK); Knapp, Roy M. (Norman, OK); Menzie, Donald E. (Norman, OK)

    1985-12-17

    Subterranean paths of water flow are impeded or changed by the facilitation of microbial growth therein. Either indigenous bacterial growth may be stimulated with nutrients or the formation may be first seeded with bacteria or their spores which inhibit fluid flow after proliferation. These methods and bacteria are usable to alter the flow of water in a waterflooded oil formation and to impede the outflow of contaminated water.

  7. A Recipe for Galaxy Formation Shaun Cole

    E-Print Network [OSTI]

    Alfonso Aragon-Salamanca; Carlos S. Frenk; Julio F. Navarro; Stephen E. Zepf

    1994-02-01

    We present a detailed prescription for how galaxy formation can be modelled in hierarchical theories of structure formation. Our model incorporates the formation and merging of dark matter halos, the shock heating and radiative cooling of baryonic gas gravitationally confined in these halos, the formation of stars regulated by the energy released by evolving stars and supernovae, the merging of galaxies within dark matter halos, and the spectral evolution of the stellar populations that are formed. The procedure that we describe is very flexible and can be applied to any hierarchical clustering theory. We explore the effects of varying the stellar initial mass function, star formation rates and galaxy merging. The results we compare with an extensive range of observational data, including the B and K galaxy luminosity functions, galaxy colours, the Tully-Fisher relation and galaxy number counts.These data strongly constrain the models and enable the relative importance of each of the physical process to be assessed. We present a broadly successful model defined by a plausible choice of parameters. This fiducial model produces a much more acceptable luminosity function than most previous studies. This is achieved through a modest rate of galaxy mergers and strong suppression of star formation in halos of low circular velocity. However, it fails to produce galaxies as red as many observed ellipticals and, compared with the observed Tully-Fisher relation, the model galaxies have circular velocities which are too large. ** uuencoded compressed postscript file containing all text and figures.**

  8. Star formation relations in nearby molecular clouds

    SciTech Connect (OSTI)

    Evans, Neal J. II; Heiderman, Amanda; Vutisalchavakul, Nalin

    2014-02-20

    We test some ideas for star formation relations against data on local molecular clouds. On a cloud by cloud basis, the relation between the surface density of star formation rate and surface density of gas divided by a free-fall time, calculated from the mean cloud density, shows no significant correlation. If a crossing time is substituted for the free-fall time, there is even less correlation. Within a cloud, the star formation rate volume and surface densities increase rapidly with the corresponding gas densities, faster than predicted by models using the free-fall time defined from the local density. A model in which the star formation rate depends linearly on the mass of gas above a visual extinction of 8 mag describes the data on these clouds, with very low dispersion. The data on regions of very massive star formation, with improved star formation rates based on free-free emission from ionized gas, also agree with this linear relation.

  9. UNIVERSITY OF CALGARY Modeling Fracture Formation on Growing Surfaces

    E-Print Network [OSTI]

    Prusinkiewicz, Przemyslaw

    UNIVERSITY OF CALGARY Modeling Fracture Formation on Growing Surfaces by Pavol Federl A THESIS Fracture Formation on Growing Surfaces" submitted by Pavol Federl in partial fulfillment This thesis describes a framework for modeling fracture formation on differentially growing, bi- layered

  10. Creating and maintaining a gas cap in tar sands formations

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Karanikas, John Michael (Houston, TX); Dinkoruk, Deniz Sumnu (Houston, TX); Wellington, Scott Lee (Bellaire, TX)

    2010-03-16

    Methods for treating a tar sands formation are disclosed herein. Methods for treating a tar sands formation may include providing heat to at least part of a hydrocarbon layer in the formation from one or more heaters located in the formation. Pressure may be allowed to increase in an upper portion of the formation to provide a gas cap in the upper portion. At least some hydrocarbons are produced from a lower portion of the formation.

  11. Mixed-mode diesel HCCI with External Mixture Formation: Preliminary...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    Mixed-mode diesel HCCI with External Mixture Formation: Preliminary Results Mixed-mode diesel HCCI with External Mixture Formation: Preliminary Results 2003 DEER Conference...

  12. Formation and Stability of Impurity "Snakes" in Tokamak Plasmas...

    Office of Scientific and Technical Information (OSTI)

    Formation and Stability of Impurity "Snakes" in Tokamak Plasmas Citation Details In-Document Search Title: Formation and Stability of Impurity "Snakes" in Tokamak Plasmas Authors:...

  13. Evidence of a halo formation mechanism in the Spallation Neutron...

    Office of Scientific and Technical Information (OSTI)

    Published Article: Evidence of a halo formation mechanism in the Spallation Neutron Source linac Title: Evidence of a halo formation mechanism in the Spallation Neutron Source...

  14. Uncovering Fundamental Ash-Formation Mechanisms and Potential...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    Uncovering Fundamental Ash-Formation Mechanisms and Potential Means to Control the Impact on DPF Performance and Engine Efficiency Uncovering Fundamental Ash-Formation Mechanisms...

  15. Energy Secretary Moniz Announces Formation of Nuclear Energy...

    Office of Environmental Management (EM)

    Formation of Nuclear Energy Tribal Working Group Energy Secretary Moniz Announces Formation of Nuclear Energy Tribal Working Group December 12, 2014 - 2:00pm Addthis News Media...

  16. The role of polymer formation during vapor phase lubrication...

    Office of Scientific and Technical Information (OSTI)

    The role of polymer formation during vapor phase lubrication of silicon. Citation Details In-Document Search Title: The role of polymer formation during vapor phase lubrication of...

  17. Internet ExplorerFirefoxSafariGoogle Chrome Readerhttp://get.adobe.com/jp/reader/

    E-Print Network [OSTI]

    Web 2014/11/07 201411 #12;1 1. 2. 2-1. 2-2. 3. 4. 5. 6. 6-1. 6-1-1. 6-1-2. 6 50 51 52 58 59 60 64 Web #12;2 WebLAN Web Web Web LAN LAN Web #12;3 Web LAN Web Internet ExplorerFirefoxSafariGoogle Chrome SSLWeb PDFAdobe Readerhttp

  18. V-176: Adobe Flash Player Memory Corruption Flaw Lets Remote Users Execute

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyThe U.S.Lacledeutilities. The Economics ofConduct Cross-Site ScriptingDepartment

  19. V-197: Adobe ColdFusion 10 WebSockets Security Bypass Vulnerability |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyThe U.S.Lacledeutilities. The Economics ofConductMultipleAccount Password

  20. T-630: Security update available for Adobe Flash Player | Department of

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCED MANUFACTURINGEnergyPlan | Department ofSUPPLEMENTSwitzerland| Department of|

  1. T-638: Security update available for Adobe Flash Player | Department of

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCED MANUFACTURINGEnergyPlan | Department ofSUPPLEMENTSwitzerland| Department

  2. T-638: Security update available for Adobe Flash Player | Department of

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LIST OF APPLICABLEStatutory Authority SustainXSystem for

  3. U-241: Adobe Flash Player Bugs Let Remote Users Execute Arbitrary Code and

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCEDInstallers/ContractorsPhotovoltaicsStateof Energy| Department of Energy 7:Obtain

  4. U-257: Adobe ColdFusion Unspecified Bug Lets Remote Users Deny Service |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCEDInstallers/ContractorsPhotovoltaicsStateof Energy| Department ofAttacks | Department

  5. V-045: Adobe ColdFusion Lets Local Users Bypass Sandbox Restrictions |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics And Statistics » USAJobs Search USAJobs SearchWater-Saving Projects |SummitVOCs|andDepartment

  6. V-069: BlackBerry Tablet OS Adobe Flash Player and Samba Multiple

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics And Statistics » USAJobs Search USAJobs SearchWater-Saving Projects1:

  7. V-110: Adobe Flash Player Bugs Let Remote Users Execute Arbitrary Code |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematics And Statistics » USAJobs Search USAJobs SearchWater-Saving Projects1:Department5:Arbitrary Code

  8. In situ oxidation of subsurface formations

    DOE Patents [OSTI]

    Beer, Gary Lee (Houston, TX); Mo, Weijian (Sugar Land, TX); Li, Busheng (Houston, TX); Shen, Chonghui (Calgary, CA)

    2011-01-11

    Methods and systems for treating a hydrocarbon containing formation described herein include providing heat to a first portion of the formation from a plurality of heaters in the first portion, producing produced through one or more production wells in a second portion of the formation, reducing or turning off heat provided to the first portion after a selected time, providing an oxidizing fluid through one or more of the heater wells in the first portion, providing heat to the first portion and the second portion through oxidation of at least some hydrocarbons in the first portion, and producing fluids through at least one of the production wells in the second portion. The produced fluids may include at least some oxidized hydrocarbons produced in the first portion.

  9. General relativity and cosmic structure formation

    E-Print Network [OSTI]

    Adamek, Julian; Durrer, Ruth; Kunz, Martin

    2015-01-01

    Numerical simulations are a versatile tool providing insight into the complicated process of structure formation in cosmology. This process is mainly governed by gravity, which is the dominant force on large scales. To date, a century after the formulation of general relativity, numerical codes for structure formation still employ Newton's law of gravitation. This approximation relies on the two assumptions that gravitational fields are weak and that they are only sourced by non-relativistic matter. While the former appears well justified on cosmological scales, the latter imposes restrictions on the nature of the "dark" components of the Universe (dark matter and dark energy) which are, however, poorly understood. Here we present the first simulations of cosmic structure formation using equations consistently derived from general relativity. We study in detail the small relativistic effects for a standard {\\Lambda}CDM cosmology which cannot be obtained within a purely Newtonian framework. Our particle-mesh N...

  10. Formation of Cyanoformaldehyde in the interstellar space

    E-Print Network [OSTI]

    Das, Ankan; Chakrabarti, Sandip K; Saha, Rajdeep; Chakrabarti, Sonali

    2013-01-01

    Cyanoformaldehyde (HCOCN) molecule has recently been suspected towards the Sagittarius B2(N) by the Green Bank telescope, though a confirmation of this observation has not yet been made. In and around a star forming region, this molecule could be formed by the exothermic reaction between two abundant interstellar species, H$_2$CO and CN. Till date, the reaction rate coefficient for the formation of this molecule is unknown. Educated guesses were used to explain the abundance of this molecule by chemical modeling. In this paper, we carried out quantum chemical calculations to find out empirical rate coefficients for the formation of HCOCN and different chemical properties during the formation of HCOCN molecules. Though HCOCN is stable against unimolecular decomposition, this gas phase molecule could be destroyed by many other means, like: ion-molecular reactions or by the effect of cosmic rays. Ion-molecular reaction rates are computed by using the capture theories. We have also included the obtained rate coef...

  11. The Formation of Primordial Luminous Objects

    E-Print Network [OSTI]

    Emanuele Ripamonti; Tom Abel

    2005-07-06

    In these lecture notes we review the current knowledge about the formation of the first luminous objects. We start from the cosmological context of hierarchical models of structure formation, and discuss the main physical processes which are believed to lead to primordial star formation, i.e. the cooling processes and the chemistry of molecules (especially H2) in a metal-free gas. We then describe the techniques and results of numerical simulations, which indicate that the masses of the first luminous objects are likely to be much larger than that of present-day stars. Finally, we discuss the scenario presented above, exposing some of the most interesting problems which are currently being investigated, such as that of the feedback effects of these objects.

  12. Planet Formation: Planet Formation: Evolution of The Solar NebulaEvolution of The Solar Nebula

    E-Print Network [OSTI]

    Herrick, Robert R.

    Planet Formation: Planet Formation: Evolution of The Solar NebulaEvolution of The Solar Nebula #12;Evolution of the Solar NebulaEvolution of the Solar Nebula 1.1. Nebula collapses into a disk 2000 KTemperatures near the Sun reach 2000 K #12;Evolution of the Solar NebulaEvolution of the Solar

  13. Unit Unit Desc Unit Unit Desc Program Program Desc OLD ACCOUNT FORMAT NEW ACCOUNT FORMAT

    E-Print Network [OSTI]

    Unit Unit Desc Unit Unit Desc Program Program Desc OLD ACCOUNT FORMAT NEW ACCOUNT FORMAT 001113 AP Old O/S A/P NonResCk 0000 General 000000 General #12;Unit Unit Desc Unit Unit Desc Program Program

  14. Formation Word/ExcelFormation Word/Excel Prsentateur:Prsentateur

    E-Print Network [OSTI]

    Vellend, Mark

    11 Formation Word/ExcelFormation Word/Excel Présentateur:Présentateur: Christian Desrochers partir de Word 2002. De légères différences peuventWord 2002. De légères différences peuvent survenir avec une version de Wordsurvenir avec une version de Word différente.différente. #12;33 Objectifs de la

  15. Factors of paleosol formation in a Late Cretaceous eolian sand sheet paleoenvironment, Marlia Formation, Southeastern Brazil

    E-Print Network [OSTI]

    Ahmad, Sajjad

    Formation, Southeastern Brazil Patrick Francisco Führ Dal' Bó a, , Giorgio Basilici a , Rômulo Simões), Brazil b IG ­ Universidade Federal do Pará, 66075-110, Belém (PA), Brazil a b s t r a c ta r t i c l e i Late Cretaceous The Marília Formation, which crops out in southeastern Brazil, is interpreted as a Late

  16. STAR FORMATION IN TWO LUMINOUS SPIRAL GALAXIES

    SciTech Connect (OSTI)

    Hunter, Deidre A.; Ashburn, Allison; Wright, Teresa; Elmegreen, Bruce G.; Rubin, Vera C.; Józsa, Gyula I. G.; Struve, Christian

    2013-10-01

    We examined star formation in two very luminous (M{sub V} = –22 to –23) Sc-type spiral galaxies, NGC 801 and UGC 2885, using ultra-deep H? images. We combine these H? images with UBV and Two-Micron All-Sky Survey JHK images and H I maps to explore the star formation characteristics of disk galaxies at high luminosity. H? traces star formation in these galaxies to 4-6 disk scale lengths, but the lack of detection of H? further out is likely due to the loss of Lyman continuum photons. Considering gravitational instabilities alone, we find that the gas and stars in the outer regions are marginally stable in an average sense, but considering dissipative gas and radial and azimuthal forcing, the outer regions are marginally unstable to forming spiral arms. Star formation is taking place in spiral arms, which are regions of locally higher gas densities. Furthermore, we have traced smooth exponential stellar disks over four magnitudes in V-band surface brightness and 4-6 disk scale lengths, in spite of a highly variable gravitational instability parameter. Thus, gravitational instability thresholds do not seem relevant to the stellar disk. One possibility for creating an exponential disk is that the molecular cloud densities and star formation rates have exponential profiles and this fact forces the stellar disk to build up such a profile. Another possibility is that the stellar disk is continuously adjusted to an exponential shape regardless of the star formation profile, for example, through global dynamical processes that scatter stars. However, such scattering processes are only known to operate in spiral systems, in which case they cannot explain the same dilemma of smooth exponential disks observed in dwarf irregular galaxies.

  17. Aromatics oxidation and soot formation in flames

    SciTech Connect (OSTI)

    Howard, J.B.; Pope, C.J.; Shandross, R.A.; Yadav, T. [Massachusetts Institute of Technology, Cambridge (United States)

    1993-12-01

    This project is concerned with the kinetics and mechanisms of aromatics oxidation and soot and fullerenes formation in flames. The scope includes detailed measurements of profiles of stable and radical species concentrations in low-pressure one-dimensional premixed flames. Intermediate species identifications and mole fractions, fluxes, and net reaction rates calculated from the measured profiles are used to test postulated reaction mechanisms. Particular objectives are to identify and to determine or confirm rate constants for the main benzene oxidation reactions in flames, and to characterize fullerenes and their formation mechanisms and kinetics.

  18. Creating fluid injectivity in tar sands formations

    DOE Patents [OSTI]

    Stegemeier, George Leo; Beer, Gary Lee; Zhang, Etuan

    2010-06-08

    Methods for treating a tar sands formation are described herein. Methods for treating a tar sands may include heating a portion of a hydrocarbon layer in the formation from one or more heaters located in the portion. The heat may be controlled to increase the permeability of at least part of the portion to create an injection zone in the portion with an average permeability sufficient to allow injection of a fluid through the injection zone. A drive fluid and/or an oxidizing fluid may be provided into the injection zone. At least some hydrocarbons are produced from the portion.

  19. Creating fluid injectivity in tar sands formations

    DOE Patents [OSTI]

    Stegemeier, George Leo; Beer, Gary Lee; Zhang, Etuan

    2012-06-05

    Methods for treating a tar sands formation are described herein. Methods for treating a tar sands may include heating a portion of a hydrocarbon layer in the formation from one or more heaters located in the portion. The heat may be controlled to increase the permeability of at least part of the portion to create an injection zone in the portion with an average permeability sufficient to allow injection of a fluid through the injection zone. A drive fluid and/or an oxidizing fluid may be provided into the injection zone. At least some hydrocarbons including mobilized hydrocarbons are produced from the portion.

  20. Induction heaters used to heat subsurface formations

    DOE Patents [OSTI]

    Nguyen, Scott Vinh (Houston, TX); Bass, Ronald M. (Houston, TX)

    2012-04-24

    A heating system for a subsurface formation includes an elongated electrical conductor located in the subsurface formation. The electrical conductor extends between at least a first electrical contact and a second electrical contact. A ferromagnetic conductor at least partially surrounds and at least partially extends lengthwise around the electrical conductor. The electrical conductor, when energized with time-varying electrical current, induces sufficient electrical current flow in the ferromagnetic conductor such that the ferromagnetic conductor resistively heats to a temperature of at least about 300.degree. C.

  1. Parallel heater system for subsurface formations

    DOE Patents [OSTI]

    Harris, Christopher Kelvin (Houston, TX); Karanikas, John Michael (Houston, TX); Nguyen, Scott Vinh (Houston, TX)

    2011-10-25

    A heating system for a subsurface formation is disclosed. The system includes a plurality of substantially horizontally oriented or inclined heater sections located in a hydrocarbon containing layer in the formation. At least a portion of two of the heater sections are substantially parallel to each other. The ends of at least two of the heater sections in the layer are electrically coupled to a substantially horizontal, or inclined, electrical conductor oriented substantially perpendicular to the ends of the at least two heater sections.

  2. Ralf Klessen: Lecture 2: 27.12.2006 Star Formation

    E-Print Network [OSTI]

    Klessen,Ralf

    efficiencyefficiency? How do globalglobal properties of the galaxy influence star formation (a locallocal process

  3. Distributed Control of Formation Flying Spacecraft Built on OA

    E-Print Network [OSTI]

    and the potential for creating fuel-efficient formation configurations rele- vant to future magnetospheric space

  4. Power systems utilizing the heat of produced formation fluid

    DOE Patents [OSTI]

    Lambirth, Gene Richard (Houston, TX)

    2011-01-11

    Systems, methods, and heaters for treating a subsurface formation are described herein. At least one method includes treating a hydrocarbon containing formation. The method may include providing heat to the formation; producing heated fluid from the formation; and generating electricity from at least a portion of the heated fluid using a Kalina cycle.

  5. La Cl informatique Formation Outlook 2000

    E-Print Network [OSTI]

    Vellend, Mark

    La Clé informatique Formation Outlook 2000 Aide-mémoire Novembre 2003 #12;Table des matières Écrire directement dans votre Outlook. Voici la méthode pour le faire. Dans le menu Outils, choisir Comptes de Hotmail apparaîtra dans la liste des comptes de Outlook. 11 #12;Mettre un arrière plan dans votre message

  6. Star Formation Histories in the Local Group

    E-Print Network [OSTI]

    Thomas M. Brown

    2004-07-09

    Deep color magnitude diagrams extending to the main sequence provide the most direct measure of the detailed star formation history in a stellar population. With large investments of observing time, HST can obtain such data for populations out to 1 Mpc, but its field of view is extremely small in comparison to the size of Local Group galaxies. This limitation severely constrains our understanding of galaxy formation. For example, the largest galaxy in the Local Group, Andromeda, offers an ideal laboratory for studying the formation of large spiral galaxies, but the galaxy shows substructure on a variety of scales, presumably due to its violent merger history. Within its remaining lifetime, HST can only sample a few sight-lines through this complex galaxy. In contrast, a wide field imager could provide a map of Andromeda's halo, outer disk, and tidal streams, revealing the spatially-dependent star formation history in each structure. The same data would enable many secondary studies, such as the age variation in Andromeda's globular cluster system, gigantic samples of variable stars, and microlensing tracers of the galaxy's dark matter distribution.

  7. Can Photo-Evaporation Trigger Planetesimal Formation?

    E-Print Network [OSTI]

    Throop, Henry

    Can Photo-Evaporation Trigger Planetesimal Formation? Henry Throop John Bally SWRI Univ.Colorado / CASA DPS 12-Oct-2004 #12;Orion Nebula Photo-evaporation by extr 4 O/B stars, UV-bright, 105 solar luminosities 2000 solar-type stars with disks Photo-evaporation (PE) by external O/B stars removes disks on 105

  8. Formation distance Stphanie Jean-Daubias

    E-Print Network [OSTI]

    Jean-Daubias, Stéphanie

    ) dans le temps et dans l'espace de l'apprenant et de l'équipe professorale 3 #12;Deux types de médias en;Formation à distance et espace Plusieurs variantes possibles enseignement entièrement à distance

  9. Facult de Sant Publique Formation continue

    E-Print Network [OSTI]

    Nesterov, Yurii

    Faculté de Santé Publique Formation continue en management des institutions de soins Programme 2011, management stratégique (UCL, ULB) CIPS p.16 > Certificat interuniversitaire en management de la qualité dans) p.19 > Certificat interuniversitaire en management médical (ULB, UCL) CIMM p.19 > Certificat

  10. Formatting Your Senior Project Get started!

    E-Print Network [OSTI]

    Arnold, Elizabeth A.

    at the bottom right of the dialog box. #12;Overall Formatting Guidelines Margins · Set all margins to 1 inch (top, bottom, left and right) · Set Header and Footer to .5 inch Font · Set size at 12 points · Choose Courier New, Times New Roman, Arial, Garamond, or Century Schoolbook. Alignment · Align text LEFT only

  11. ACOUSTIC FORMING FOR ENHANCED DEWATERING AND FORMATION

    SciTech Connect (OSTI)

    Cyrus K Aidun

    2007-11-30

    The next generation of forming elements based on acoustic excitation to increase drainage and enhances formation both with on-line control and profiling capabilities has been investigated in this project. The system can be designed and optimized based on the fundamental experimental and computational analysis and investigation of acoustic waves in a fiber suspension flow and interaction with the forming wire.

  12. Varying heating in dawsonite zones in hydrocarbon containing formations

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Xie, Xueying (Houston, TX); Miller, David Scott (Katy, TX)

    2009-07-07

    A method for treating an oil shale formation comprising dawsonite includes assessing a dawsonite composition of one or more zones in the formation. Heat from one or more heaters is provided to the formation such that different amounts of heat are provided to zones with different dawsonite compositions. The provided heat is allowed to transfer from the heaters to the formation. Fluids are produced from the formation.

  13. IMPACTS OF BIOFILM FORMATION ON CELLULOSE FERMENTATION

    SciTech Connect (OSTI)

    Leschine, Susan

    2009-10-31

    This project addressed four major areas of investigation: i) characterization of formation of Cellulomonas uda biofilms on cellulose; ii) characterization of Clostridium phytofermentans biofilm development; colonization of cellulose and its regulation; iii) characterization of Thermobifida fusca biofilm development; colonization of cellulose and its regulation; and iii) description of the architecture of mature C. uda, C. phytofermentans, and T. fusca biofilms. This research is aimed at advancing understanding of biofilm formation and other complex processes involved in the degradation of the abundant cellulosic biomass, and the biology of the microbes involved. Information obtained from these studies is invaluable in the development of practical applications, such as the single-step bioconversion of cellulose-containing residues to fuels and other bioproducts. Our results have clearly shown that cellulose-decomposing microbes rapidly colonize cellulose and form complex structures typical of biofilms. Furthermore, our observations suggest that, as cells multiply on nutritive surfaces during biofilms formation, dramatic cell morphological changes occur. We speculated that morphological changes, which involve a transition from rod-shaped cells to more rounded forms, might be more apparent in a filamentous microbe. In order to test this hypothesis, we included in our research a study of biofilm formation by T. fusca, a thermophilic cellulolytic actinomycete commonly found in compost. The cellulase system of T. fusca has been extensively detailed through the work of David Wilson and colleagues at Cornell, and also, genome sequence of a T. fusca strain has been determine by the DOE Joint Genome Institute. Thus, T. fusca is an excellent subject for studies of biofilm development and its potential impacts on cellulose degradation. We also completed a study of the chitinase system of C. uda. This work provided essential background information for understanding how C. uda colonizes and degrades insoluble substrates. Major accomplishments of the project include: • Development of media containing dialysis tubing (described by the manufacturer as “regenerated cellulose”) as sole carbon and energy source and a nutritive surface for the growth of cellulolytic bacteria, and development of various microscopic methods to image biofilms on dialysis tubing. • Demonstration that cultures of C. phytofermentans, an obligate anaerobe, C. uda, a facultative aerobe, and T. fusca, a filamentous aerobe, formed microbial communities on the surface of dialysis tubing, which possessed architectural features and functional characteristics typical of biofilms. • Demonstration that biofilm formation on the nutritive surface, cellulose, involves a complex developmental processes, including colonization of dialysis tubing, formation of cell clusters attached to the nutritive surface, cell morphological changes, formation of complex structures embedded in extracellular polymeric matrices, and dispersal of biofilm communities as the nutritive surface is degraded. • Determination of surface specificity and regulatory aspects of biofilm formation by C. phytofermentans, C. uda, and T. fusca. • Demonstration that biofilm formation by T. fusca forms an integral part of the life cycle of this filamentous cellulolytic bacterium, including studies on the role of mycelial pellet formation in the T. fusca life cycle and a comparison of mycelial pellets to surface-attached T. fusca biofilms. • Characterization of T. fusca biofilm EPS, including demonstration of a functional role for EPS constituents. • Correlation of T. fusca developmental life cycle and cellulase gene expression.

  14. (Non) formation of methanol by direct hydrogenation of formate on copper catalysts

    SciTech Connect (OSTI)

    Yang, Yong; Mims, Charles A.; Disselkamp, Robert S.; Kwak, Ja Hun; Peden, Charles HF; Campbell, C. T.

    2010-10-14

    We have attempted to hydrogenate adsorbed formate species on copper catalysts to probe the importance of this postulated mechanistic step in methanol synthesis. Surface formate coverages up to 0.25 were produced at temperatures between 413K and 453K on supported (Cu/SiO2) copper and unsupported copper catalysts. The adlayers were produced by various methods including (1) steady state catalytic conditions in CO2-H2 (3:1, 6 bar) atmospheres, and (2) by exposure of the catalysts to formic acid. As reported in earlier work, the catalytic surface at steady state contains bidentate formate species with coverages up to saturation levels of ~ 0.25 at the low temperatures of this study. The reactivity of these formate adlayers was investigated at relevant reaction temperatures in atmospheres containing up to 6 bar H2 partial pressure by simultaneous mass spectrometry (MS) and infrared (IR) spectroscopy measurements. The yield of methanol during the attempted hydrogenation (“titration”) of these adlayers was insignificant (<0.2 mol % of the formate adlayer) even in dry hydrogen partial pressures up to 6 bar. Hydrogen titration of formate species produced from formic acid also failed to produce significant quantities of methanol, and attempted titration in gases consisting of CO-hydrogen mixtures or dry CO2 were also unproductive. The formate decomposition kinetics, measured by IR, were also unaffected by these changes in the gas composition. Similar experiments on unsupported copper also failed to show any methanol. From these results, we conclude that methanol synthesis on copper cannot result from the direct hydrogenation of (bidentate) formate species in simple steps involving adsorbed H species alone. Furthermore, experiments performed on both supported (Cu/SiO2) and unsupported copper catalysts gave similar results implying that the methanol synthesis reaction mechanism only involves metal surface chemistry. Pre-exposure of the bidentate formate adlayer to oxidation by O2 or N2O produces a change to a monodentate configuration. Attempted titration of this monodentate formate/O coadsorbed layer in dry hydrogen produces significant quantities of methanol, although decomposition of formate to carbon dioxide and hydrogen remains the dominant reaction pathway. Simultaneous production of water is also observed during this titration as the copper surface is re-reduced. These results indicate that co-adsorbates related to surface oxygen or water-derived species may be critical to methanol production on copper, perhaps assisting in the hydrogenation of adsorbed formate to adsorbed methoxyl.

  15. Environmental Surveillance at Los Alamos during 2007

    SciTech Connect (OSTI)

    2008-09-30

    Environmental Surveillance at Los Alamos reports are prepared annually by the Los Alamos National Laboratory (the Laboratory) Environmental Directorate, as required by US Department of Energy Order 450.1, General Environmental Protection Program, and US Department of Energy Order 231.1A, Environment, Safety, and Health Reporting. These annual reports summarize environmental data that are used to determine compliance with applicable federal, state, and local environmental laws and regulations, executive orders, and departmental policies. Additional data, beyond the minimum required, are also gathered and reported as part of the Laboratory’s efforts to ensure public safety and to monitor environmental quality at and near the Laboratory. Chapter 1 provides an overview of the Laboratory’s major environmental programs and explains the risks and the actions taken to reduce risks at the Laboratory from environmental legacies and waste management operations. Chapter 2 reports the Laboratory’s compliance status for 2007. Chapter 3 provides a summary of the maximum radiological dose the public and biota populations could have potentially received from Laboratory operations and discusses chemical exposures. The environmental surveillance and monitoring data are organized by environmental media (Chapter 4, air; Chapters 5 and 6, water and sediments; Chapter 7, soils; and Chapter 8, foodstuffs and biota) in a format to meet the needs of a general and scientific audience. Chapter 9 provides a summary of the status of environmental restoration work around LANL. A glossary and a list of acronyms and abbreviations are in the back of the report. Appendix A explains the standards for environmental contaminants, Appendix B explains the units of measurements used in this report, Appendix C describes the laboratory’s technical areas and their associated programs, and Appendix D provides web links to more information. In printed copies of this report or Executive Summary, we have also enclosed a compact disc with a copy of the full report in Adobe Acrobat (PDF) form and detailed supplemental tables of data from 2007 in Microsoft Excel format. These files are also available for download from the web (http://www.lanl.gov/community-environment/environmental- stewardship/environmental-report.php).

  16. NOx Formation in a Premixed Syngas Flame

    SciTech Connect (OSTI)

    Yilmaz, S.L. (University of Pittsburgh, Pittsburgh, PA); Givi, P. (University of Pittsburgh, Pittsburgh, PA); Strakey, P.; Casleton, K.

    2006-11-01

    Reduction of NOx is a subject of significant current interest in stationary gas turbines. The objective of this study is to examine the effects of turbulence on non-thermal NOx formation in a syngas flame. This is archived by a detailed parametric study via PDF simulations of a partially stirred reactor and a dumped axisymmetric premixed flame. Several different detailed and reduced kinetics schemes are considered. The simulated results demonstrate the strong dependence of combustion process on turbulence. It is shown that the amount of NOx formation is significantly influenced by the inlet conditions. That is, the turbulence intensity can be tweaked to attain optimal ultra-low NOx emissions at a given temperature.

  17. Reconstructing the Star Formation Histories of Galaxies

    E-Print Network [OSTI]

    Uta Fritze; Thomas Lilly

    2007-01-15

    We present a methodological study to find out how far back and to what precision star formation histories of galaxies can be reconstructed from CMDs, from integrated spectra and Lick indices, and from integrated multi-band photometry. Our evolutionary synthesis models GALEV allow to describe the evolution of galaxies in terms of all three approaches and we have assumed typical observational uncertainties for each of them and then investigated to what extent and accuracy different star formation histories can be discriminated. For a field in the LMC bar region with both a deep CMD from HST observations and a trailing slit spectrum across exactly the same field of view we could test our modelling results against real data.

  18. Low voltage arc formation in railguns

    DOE Patents [OSTI]

    Hawke, Ronald S. (Livermore, CA)

    1987-01-01

    A low voltage plasma arc is first established across the rails behind the projectile by switching a low voltage high current source across the rails to establish a plasma arc by vaporizing a fuse mounted on the back of the projectile, maintaining the voltage across the rails below the railgun breakdown voltage to prevent arc formation ahead of the projectile. After the plasma arc has been formed behind the projectile a discriminator switches the full energy bank across the rails to accelerate the projectile. A gas gun injector may be utilized to inject a projectile into the breech of a railgun. The invention permits the use of a gas gun or gun powder injector and an evacuated barrel without the risk of spurious arc formation in front of the projectile.

  19. Low voltage arc formation in railguns

    DOE Patents [OSTI]

    Hawke, R.S.

    1985-08-05

    A low voltage plasma arc is first established across the rails behind the projectile by switching a low voltage high current source across the rails to establish a plasma arc by vaporizing a fuse mounted on the back of the projectile, maintaining the voltage across the rails below the railgun breakdown voltage to prevent arc formation ahead of the projectile. After the plasma arc has been formed behind the projectile a discriminator switches the full energy bank across the rails to accelerate the projectile. A gas gun injector may be utilized to inject a projectile into the breech of a railgun. The invention permits the use of a gas gun or gun powder injector and an evacuated barrel without the risk of spurious arc formation in front of the projectile.

  20. Low voltage arc formation in railguns

    DOE Patents [OSTI]

    Hawke, R.S.

    1987-11-17

    A low voltage plasma arc is first established across the rails behind the projectile by switching a low voltage high current source across the rails to establish a plasma arc by vaporizing a fuse mounted on the back of the projectile, maintaining the voltage across the rails below the railgun breakdown voltage to prevent arc formation ahead of the projectile. After the plasma arc has been formed behind the projectile a discriminator switches the full energy bank across the rails to accelerate the projectile. A gas gun injector may be utilized to inject a projectile into the breech of a railgun. The invention permits the use of a gas gun or gun powder injector and an evacuated barrel without the risk of spurious arc formation in front of the projectile. 2 figs.

  1. Shocks, Star Formation, and the JWST

    E-Print Network [OSTI]

    Gusdorf, Antoine

    2015-01-01

    The interstellar medium (ISM) is constantly evolving due to unremitting injection of energy in various forms. Energetic radiation transfers energy to the ISM: from the UV photons, emitted by the massive stars, to X- and $\\gamma$-ray ones. Cosmic rays are another source of energy. Finally, mechanical energy is injected through shocks or turbulence. Shocks are ubiquitous in the interstellar medium of galaxies. They are associated to star formation (through jets and bipolar outflows), life (via stellar winds), and death (in AGB stellar winds or supernovae explosion). The dynamical processes leading to the formation of molecular clouds also generate shocks where flows of interstellar matter collide. Because of their ubiquity, the study of interstellar shocks is also a useful probe to the other mechanisms of energy injection in the ISM. This study must be conducted in order to understand the evolution of the ISM as a whole, and to address various questions: what is the peculiar chemistry associated to shocks, and ...

  2. Nanodot formation induced by femtosecond laser irradiation

    SciTech Connect (OSTI)

    Abere, M. J.; Kang, M.; Goldman, R. S.; Yalisove, S. M. [Department of Materials Science and Engineering, University of Michigan, Ann Arbor, Michigan 48109 (United States); Chen, C. [Applied Physics Program, University of Michigan, Ann Arbor, Michigan 48109 (United States); Rittman, D. R. [Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, Michigan 48109 (United States); Phillips, J. D. [Department of Electrical Engineering and Computer Science, University of Michigan, Ann Arbor, Michigan 48109 (United States); Torralva, B. [Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan 48109 (United States)

    2014-10-20

    The femtosecond laser generation of ZnSe nanoscale features on ZnSe surfaces was studied. Irradiation with multiple exposures produces 10–100?nm agglomerations of nanocrystalline ZnSe while retaining the original single crystal structure of the underlying material. The structure of these nanodots was verified using a combination of scanning transmission electron microscopy, scanning electron microscopy, and atomic force microscopy. The nanodots continue to grow hours after irradiation through a combination of bulk and surface diffusion. We suggest that in nanodot formation the result of ultrafast laser induced point defect formation is more than an order of magnitude below the ZnSe ultrafast melt threshold fluence. This unique mechanism of point defect injection will be discussed.

  3. Naked Singularity formation in scalar field collapse

    E-Print Network [OSTI]

    Rituparno Goswami; Pankaj S Joshi

    2004-10-28

    We construct here a class of collapsing scalar field models with a non-zero potential, which result in a naked singularity as collapse end state. The weak energy condition is satisfied by the collapsing configuration. It is shown that physically it is the rate of collapse that governs either the black hole or naked singularity formation as the final state for the dynamical evolution. It is seen that the cosmic censorship is violated in dynamical scalar field collapse.

  4. Galactosynthesis: Halo Histories, Star Formation, and Disks

    E-Print Network [OSTI]

    Ari Buchalter; Raul Jimenez; Marc Kamionkowski

    2000-06-01

    We investigate the effects of a variety of ingredients that must enter into a realistic model for disk-galaxy formation, focusing primarily on the Tully-Fisher (TF) relation and its scatter in several wavebands. Our main findings are: (a) the slope, normalization, and scatter of the TF relation across various wavebands is determined {\\em both} by halo properties and star formation in the disk; (b) TF scatter owes primarily to the spread in formation redshifts. The scatter can be measurably reduced by chemical evolution, and also in some cases by the weak anti-correlation between peak height and spin; (c) multi-wavelength constraints can be important in distinguishing between models which appear to fit the TF relation in I or K; (d) successful models seem to require that the bulk of disk formation cannot occur too early (z>2) or too late (z<0.5), and are inconsistent with high values of $\\Omega_0$; (e) a realistic model with the above ingredients can reasonably reproduce the observed z=0 TF relation in {\\em all} bands (B, R, I, and K). It can also account for the z=1 B-band TF relation and yield rough agreement with the local B and K luminosity functions and B-band surface-brightness--magnitude relation. The remarkable agreement with observations suggests that the amount of gas that is expelled or poured into a disk galaxy must be small, and that the specific angular momentum of the baryons must roughly equal that of the halo; there is little room for angular momentum transfer. In an appendix we present analytic fits to stellar-population synthesis models.

  5. Carboxylic acid accelerated formation of diesters

    DOE Patents [OSTI]

    Tustin, G.C.; Dickson, T.J.

    1998-04-28

    This invention pertains to accelerating the rate of formation of 1,1-dicarboxylic esters from the reaction of an aldehyde with a carboxylic acid anhydride or a ketene in the presence of a non-iodide containing a strong Bronsted acid catalyst by the addition of a carboxylic acid at about one bar pressure and between about 0 and 80 C in the substantial absence of a hydrogenation or carbonylation catalyst.

  6. Galaxy Structure, Dark Matter, and Galaxy Formation

    E-Print Network [OSTI]

    David H. Weinberg

    1996-10-01

    The structure of galaxies, the nature of dark matter, and the physics of galaxy formation were the interlocking themes of DM 1996: Dark and Visible Matter in Galaxies and Cosmological Implications. In this conference summary report, I review recent observational and theoretical advances in these areas, then describe highlights of the meeting and discuss their implications. I include as an appendix the lyrics of The Dark Matter Rap: A Cosmological History for the MTV Generation.

  7. Production from multiple zones of a tar sands formation

    DOE Patents [OSTI]

    Karanikas, John Michael; Vinegar, Harold J

    2013-02-26

    A method for treating a tar sands formation includes providing heat to at least part of a hydrocarbon layer in the formation from a plurality of heaters located in the formation. The heat is allowed to transfer from the heaters to at least a portion of the formation. Fluids are produced from the formation through at least one production well that is located in at least two zones in the formation. The first zone has an initial permeability of at least 1 darcy. The second zone has an initial of at most 0.1 darcy. The two zones are separated by a substantially impermeable barrier.

  8. On star formation in primordial protoglobular clouds

    E-Print Network [OSTI]

    Paolo Padoan; Raul Jimenez; Bernard Jones

    1996-04-11

    Using a new physical model for star formation (Padoan 1995) we have tested the possibility that globular clusters (GCs) are formed from primordial mass fluctuations, whose mass scale ($10^8$ - $10^9$ M$_{\\odot}$) is selected out of a CDM spectrum by the mechanism of non-equilibrium formation of $H_2$. We show that such clouds are able to convert about 0.003 of their total mass into a bound system (GC) and about 0.02 into halo stars. The metal enriched gas is dispersed away from the GC by supernova explosions and forms the galactic disk. These mass ratios between GCs, halo and disk depend on the predicted IMF which is a consequence of the universal statistics of fluid turbulence. They also depend on the ratio of baryonic over non-baryonic mass ,$X_b$, and are comparable with the values observed in typical spiral galaxies for $X_b \\approx 0.1-0.2$. The computed mass and radius for a GC ( $5\\times 10^5$ M$_{\\odot}$ and 30 pc) are in good agreement with the average values in the Galaxy. The model predicts an exponential cut off in the stellar IMF below 0.1 M$_{\\odot}$ in GCs and 0.6 M$_{\\odot}$ in the halo. The quite massive star formation in primordial clouds leads to a large number of supernovae and to a high blue luminosity during the first two Gyr of the life of every galaxy.

  9. General relativity and cosmic structure formation

    E-Print Network [OSTI]

    Julian Adamek; David Daverio; Ruth Durrer; Martin Kunz

    2015-09-05

    Numerical simulations are a versatile tool providing insight into the complicated process of structure formation in cosmology. This process is mainly governed by gravity, which is the dominant force on large scales. To date, a century after the formulation of general relativity, numerical codes for structure formation still employ Newton's law of gravitation. This approximation relies on the two assumptions that gravitational fields are weak and that they are only sourced by non-relativistic matter. While the former appears well justified on cosmological scales, the latter imposes restrictions on the nature of the "dark" components of the Universe (dark matter and dark energy) which are, however, poorly understood. Here we present the first simulations of cosmic structure formation using equations consistently derived from general relativity. We study in detail the small relativistic effects for a standard {\\Lambda}CDM cosmology which cannot be obtained within a purely Newtonian framework. Our particle-mesh N-body code computes all six degrees of freedom of the metric and consistently solves the geodesic equation for particles, taking into account the relativistic potentials and the frame-dragging force. This conceptually clean approach is very general and can be applied to various settings where the Newtonian approximation fails or becomes inaccurate, ranging from simulations of models with dynamical dark energy or warm/hot dark matter to core collapse supernova explosions.

  10. Stratigraphy of the Calvert Bluff Formation of the Wilcox Group, Brazos County, Texas 

    E-Print Network [OSTI]

    May, Audrey Gail

    1994-01-01

    Wilcox Group sediments are classified into three main formations: a lower Hooper Formation, a middle Simsboro Formation, and an upper Calvert Bluff Formation. The Calvert Bluff and Simsboro formations have been interpreted ...

  11. Dynamic and thermal control of an electromagnetic formation flight testbed

    E-Print Network [OSTI]

    Neave, Matthew D. (Matthew David)

    2005-01-01

    Formation flight of multiple spacecraft is an emerging method for completing complex space missions in an efficient manner. A limitation found in maintaining such formations is the need for precise control at all times. ...

  12. Development of Large Format Lithium Ion Cells with Higher Energy...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    Large Format Lithium Ion Cells with Higher Energy Density Exceeding 500WhL Development of Large Format Lithium Ion Cells with Higher Energy Density Exceeding 500WhL 2012 DOE...

  13. A first site of galaxy cluster formation: complete spectroscopy...

    Office of Scientific and Technical Information (OSTI)

    A first site of galaxy cluster formation: complete spectroscopy of a protocluster at z 6.01 Citation Details In-Document Search Title: A first site of galaxy cluster formation:...

  14. Galaxy Formation and Evolution. II. Energy Balance, Star Formation and Feed-back

    E-Print Network [OSTI]

    Fulvio Buonomo; Giovanni Carraro; Cesare Chiosi; Cesario Lia

    1999-09-13

    In this paper we present a critical discussion of the algorithms commonly used in N-body simulations of Galaxy Formation to deal with the energy equation governing heating and cooling, to model star formation and the star formation rate, and to account for energy feed-back from stars. First, we propose our technique for solving the energy equation in presence of heating and cooling, which includes some difference with respect to the standard semi-implicit technique. Second, we examine the current criteria for the onset of the star formation activity. We suggest a new approach, in which star formaiton is let depend on the total mass density - baryonic (gas and stars) and dark matter - of the system and on the metal-dependent cooling efficiency. Third, we check and discuss the separate effects of energy (and mass) feed-back from several sources - namely supernovae, stellar winds from massive stars, and UV flux from the same objects. All the simulations are performed in the framework of the formation and evolution of a disk galaxy. We show that the inclusion of these physical phenomena has a signigicant impact on the evolution of the galaxy model.

  15. RAPID DUST FORMATION IN NOVAE: THE SPEED CLASS—FORMATION TIMESCALE CORRELATION EXPLAINED

    SciTech Connect (OSTI)

    Williams, S. C.; Bode, M. F.; Darnley, M. J.; Evans, A.; Zubko, V.; Shafter, A. W.

    2013-11-10

    Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships between speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted short-ward of the Lyman limit. The rate at which the spectrum evolves also depends on the speed class. We have therefore refined the simple model by assuming photons at energies higher than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites, therefore preventing these photons reaching the nucleation sites. With this refinement the dust formation timescale is theoretically dependent on speed class and the results of our theoretical modification agree well with the observational data. We consider two types of carbon-based dust, graphite and amorphous carbon, with both types producing similar relationships. Our results can be used to predict when dust will form in a nova of a given speed class and hence when observations should optimally be taken to detect the onset of dust formation.

  16. Energy-Driven Pattern Formation Robert V. Kohn

    E-Print Network [OSTI]

    Energy-Driven Pattern Formation Robert V. Kohn Grad Student and Postdoc Seminar April 22, 2011 Robert V. Kohn Energy-Driven Pattern Formation #12;Overview What is energy-driven pattern formation? Hard by singular perturbation Statics: minimum energy scaling laws Dynamics: patterns induced by steepest

  17. Pattern formation in drying drops Robert D. Deegan*

    E-Print Network [OSTI]

    Deegan, Robert

    , Chicago, Illinois 60637 Received 24 November 1998 Ring formation in an evaporating sessile dropPattern formation in drying drops Robert D. Deegan* James Franck Institute, 5640 South Ellis Avenue. Here I show that the drop itself can generate one of the essential conditions for ring formation

  18. Heating subsurface formations by oxidizing fuel on a fuel carrier

    DOE Patents [OSTI]

    Costello, Michael; Vinegar, Harold J.

    2012-10-02

    A method of heating a portion of a subsurface formation includes drawing fuel on a fuel carrier through an opening formed in the formation. Oxidant is supplied to the fuel at one or more locations in the opening. The fuel is combusted with the oxidant to provide heat to the formation.

  19. DEFORMATION OF THE HURRICANE MOUNTAIN FORMATION MELANGE ALONG TOMHEGAN AND

    E-Print Network [OSTI]

    Beane, Rachel J.

    DEFORMATION OF THE HURRICANE MOUNTAIN FORMATION MELANGE ALONG TOMHEGAN AND COLD STREAMS, WEST through Acadian deformation recorded in foliated pelites of the Hurricane Mountain Formation in west central Maine. The Hurricane Mountain Formation is a melange with a grey sulfidic slate- to gneiss- matrix

  20. Interoperability format translation and transformation between IFC architectural design file and simulation file formats

    DOE Patents [OSTI]

    Chao, Tian-Jy; Kim, Younghun

    2015-01-06

    Automatically translating a building architecture file format (Industry Foundation Class) to a simulation file, in one aspect, may extract data and metadata used by a target simulation tool from a building architecture file. Interoperability data objects may be created and the extracted data is stored in the interoperability data objects. A model translation procedure may be prepared to identify a mapping from a Model View Definition to a translation and transformation function. The extracted data may be transformed using the data stored in the interoperability data objects, an input Model View Definition template, and the translation and transformation function to convert the extracted data to correct geometric values needed for a target simulation file format used by the target simulation tool. The simulation file in the target simulation file format may be generated.

  1. Interoperability format translation and transformation between IFC architectural design file and simulation file formats

    DOE Patents [OSTI]

    Chao, Tian-Jy; Kim, Younghun

    2015-02-03

    Automatically translating a building architecture file format (Industry Foundation Class) to a simulation file, in one aspect, may extract data and metadata used by a target simulation tool from a building architecture file. Interoperability data objects may be created and the extracted data is stored in the interoperability data objects. A model translation procedure may be prepared to identify a mapping from a Model View Definition to a translation and transformation function. The extracted data may be transformed using the data stored in the interoperability data objects, an input Model View Definition template, and the translation and transformation function to convert the extracted data to correct geometric values needed for a target simulation file format used by the target simulation tool. The simulation file in the target simulation file format may be generated.

  2. Bistatic SAR: Signal Processing and Image Formation.

    SciTech Connect (OSTI)

    Wahl, Daniel E.; Yocky, David A.

    2014-10-01

    This report describes the significant processing steps that were used to take the raw recorded digitized signals from the bistatic synthetic aperture RADAR (SAR) hardware built for the NCNS Bistatic SAR project to a final bistatic SAR image. In general, the process steps herein are applicable to bistatic SAR signals that include the direct-path signal and the reflected signal. The steps include preprocessing steps, data extraction to for a phase history, and finally, image format. Various plots and values will be shown at most steps to illustrate the processing for a bistatic COSMO SkyMed collection gathered on June 10, 2013 on Kirtland Air Force Base, New Mexico.

  3. Globular Cluster Formation in M82

    E-Print Network [OSTI]

    S. J. Lipscy; P. Plavchan

    2003-11-12

    We present high resolution mid-infrared (mid-IR; 11.7 and 17.65 micron) maps of the central 400 pc region of the starburst galaxy M82. Seven star forming clusters are identified which together provide ~ 15% of the total mid-IR luminosity of the galaxy. Combining the mid-IR data with thermal radio measurements and near- and mid-IR line emission, we find that these young stellar clusters have inferred masses and sizes comparable to globular clusters. At least 20% of the star formation in M82 is found to occur in super-star clusters.

  4. Solar cell contact formation using laser ablation

    DOE Patents [OSTI]

    Harley, Gabriel; Smith, David D.; Cousins, Peter John

    2015-07-21

    The formation of solar cell contacts using a laser is described. A method of fabricating a back-contact solar cell includes forming a poly-crystalline material layer above a single-crystalline substrate. The method also includes forming a dielectric material stack above the poly-crystalline material layer. The method also includes forming, by laser ablation, a plurality of contacts holes in the dielectric material stack, each of the contact holes exposing a portion of the poly-crystalline material layer; and forming conductive contacts in the plurality of contact holes.

  5. Solar cell contact formation using laser ablation

    DOE Patents [OSTI]

    Harley, Gabriel; Smith, David D.; Cousins, Peter John

    2014-07-22

    The formation of solar cell contacts using a laser is described. A method of fabricating a back-contact solar cell includes forming a poly-crystalline material layer above a single-crystalline substrate. The method also includes forming a dielectric material stack above the poly-crystalline material layer. The method also includes forming, by laser ablation, a plurality of contacts holes in the dielectric material stack, each of the contact holes exposing a portion of the poly-crystalline materiat layer; and forming conductive contacts in the plurality of contact holes.

  6. Solar cell contact formation using laser ablation

    DOE Patents [OSTI]

    Harley, Gabriel; Smith, David; Cousins, Peter

    2012-12-04

    The formation of solar cell contacts using a laser is described. A method of fabricating a back-contact solar cell includes forming a poly-crystalline material layer above a single-crystalline substrate. The method also includes forming a dielectric material stack above the poly-crystalline material layer. The method also includes forming, by laser ablation, a plurality of contacts holes in the dielectric material stack, each of the contact holes exposing a portion of the poly-crystalline material layer; and forming conductive contacts in the plurality of contact holes.

  7. result formats | OpenEI Community

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowa (UtilityMichigan)data bookresult formats Home Jweers's picture Submitted

  8. 788 J. Phys. Chem. 1985,89, 788-797 sites of hydrogen-bonded hydroxyls.13 Formate formation caused

    E-Print Network [OSTI]

    Simons, Jack

    788 J. Phys. Chem. 1985,89, 788-797 sites of hydrogen-bonded hydroxyls.13 Formate formation caused surface carbonates to disappear and did not displace the isolated hydroxyls, suggesting that the formate and methoxy groups caused the isolated hydroxyls to disappear, indicating that these species were adsorbed

  9. Communication n 219 Atelier 21 : Formation au mtier du soin En quoi l'universitarisation de la formation infirmire

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    infirmier basé sur le développement des compétences. Nous avons choisi de mettre en exergue une pratique référentiels d'activités, de compétences et de formation infirmière. Mots clés : infirmier(ère), formation conduisant au diplôme d'état d'infirmier. Le référentiel de formation a comme enjeu une autre définition du

  10. 2 Star formation and outflows: an overview 2.1 The current picture of lowmass star formation

    E-Print Network [OSTI]

    Stanke, Thomas

    #24; star is not yet high enough for hydrogen fusion at the time when accretion dies out temperature is high enough for hydrogen fusion, the star #12; 12 2 STAR FORMATION AND OUTFLOWS: AN OVERVIEW11 2 Star formation and outflows: an overview 2.1 The current picture of low­mass star formation

  11. Formate brines -- New fluids for drilling and completions

    SciTech Connect (OSTI)

    Ramsey, M.S.; Shipp, J.A.

    1996-01-01

    The term ``formate brines`` refers broadly to three primary compounds dissolved in water -- sodium formate (NaCOOH), potassium formate (KCOOH) and cesium formate (CsCOOH). Each is chemically classified as an alkali-metal salt of formic acid. They offer properties that in many respects are superior to their predecessors, halide brines such as zinc bromide and calcium bromide, without the undesirable side effects of those more common halide brine systems. This article introduces the technology and provides an overview of published work to date regarding formates.

  12. Magnetic Fields in Population III Star Formation

    SciTech Connect (OSTI)

    Turk, Matthew J.; Oishi, Jeffrey S.; Abel, Tom; Bryan, Greg

    2012-02-22

    We study the buildup of magnetic fields during the formation of Population III star-forming regions, by conducting cosmological simulations from realistic initial conditions and varying the Jeans resolution. To investigate this in detail, we start simulations from identical initial conditions, mandating 16, 32 and 64 zones per Jeans length, and studied the variation in their magnetic field amplification. We find that, while compression results in some amplification, turbulent velocity fluctuations driven by the collapse can further amplify an initially weak seed field via dynamo action, provided there is sufficient numerical resolution to capture vortical motions (we find this requirement to be 64 zones per Jeans length, slightly larger than, but consistent with previous work run with more idealized collapse scenarios). We explore saturation of amplification of the magnetic field, which could potentially become dynamically important in subsequent, fully-resolved calculations. We have also identified a relatively surprising phenomena that is purely hydrodynamic: the higher-resolved simulations possess substantially different characteristics, including higher infall-velocity, increased temperatures inside 1000 AU, and decreased molecular hydrogen content in the innermost region. Furthermore, we find that disk formation is suppressed in higher-resolution calculations, at least at the times that we can follow the calculation. We discuss the effect this may have on the buildup of disks over the accretion history of the first clump to form as well as the potential for gravitational instabilities to develop and induce fragmentation.

  13. DILUTE SURFACTANT METHODS FOR CARBONATE FORMATIONS

    SciTech Connect (OSTI)

    Kishore K. Mohanty

    2004-01-01

    There are many carbonate reservoirs in US (and the world) with light oil and fracture pressure below its minimum miscibility pressure (or reservoir may be naturally fractured). Many carbonate reservoirs are naturally fractured. Waterflooding is effective in fractured reservoirs, if the formation is water-wet. Many fractured carbonate reservoirs, however, are mixed-wet and recoveries with conventional methods are low (less than 10%). Thermal and miscible tertiary recovery techniques are not effective in these reservoirs. Surfactant flooding (or huff-n-puff) is the only hope, yet it was developed for sandstone reservoirs in the past. The goal of this research is to evaluate dilute (hence relatively inexpensive) surfactant methods for carbonate formations and identify conditions under which they can be effective. Anionic surfactants (SS-6656, Alfoterra 35, 38, 63,65,68) have been identified which can change the wettability of the calcite surface to intermediate/water-wet condition as well or better than the cationic surfactant DTAB with a West Texas crude oil in the presence of Na{sub 2}CO{sub 3}. All the carbonate surfaces (Lithographic Limestone, Marble, Dolomite and Calcite) show similar behavior with respect to wettability alteration with surfactant 4-22. Anionic surfactants (5-166, Alfoterra-33 and Alfoterra-38 and Alfoterra-68), which lower the interfacial tension with a West Texas crude oil to very low values (<10{sup -2} nM/m), have also been identified. Plans for the next quarter include conducting wettability, mobilization, and imbibition studies.

  14. REVISITING JOVIAN-RESONANCE INDUCED CHONDRULE FORMATION

    SciTech Connect (OSTI)

    Nagasawa, M. [Interactive Research Center of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551 (Japan); Tanaka, K. K.; Tanaka, H. [Institute of Low Temperature Science, Hokkaido University, Kita-19, Nishi-8, Kita-ku, Sapporo 060-0819 (Japan); Nakamoto, T. [Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551 (Japan); Miura, H. [Graduate School of Natural Sciences, Nagoya City University, 1 Yamanohata, Mizuho-cho, Mizuho-ku, Nagoya 467-8501 (Japan); Yamamoto, T., E-mail: nagasawa.m.ad@m.titech.ac.jp [Center for Planetary Science, Kobe University, 7-1-48 Minamimachi, Minatojima, Chuo-ku, Kobe 650-0047 (Japan)

    2014-10-10

    It is proposed that planetesimals perturbed by Jovian mean-motion resonances are the source of shock waves that form chondrules. It is considered that this shock-induced chondrule formation requires the velocity of the planetesimal relative to the gas disk to be on the order of ? 7 km s{sup –1} at 1 AU. In previous studies on planetesimal excitation, the effects of Jovian mean-motion resonance together with the gas drag were investigated, but the velocities obtained were at most 8 km s{sup –1} in the asteroid belt, which is insufficient to account for the ubiquitous existence of chondrules. In this paper, we reexamine the effect of Jovian resonances and take into account the secular resonance in the asteroid belt caused by the gravity of the gas disk. We find that the velocities relative to the gas disk of planetesimals a few hundred kilometers in size exceed 12 km s{sup –1}, and that this is achieved around the 3:1 mean-motion resonance. The heating region is restricted to a relatively narrowband between 1.5 AU and 3.5 AU. Our results suggest that chondrules were produced effectively in the asteroid region after Jovian formation. We also find that many planetesimals are scattered far beyond Neptune. Our findings can explain the presence of crystalline silicate in comets if the scattered planetesimals include silicate dust processed by shock heating.

  15. Formation and polymerization of cyclic disilsesquioxanes

    SciTech Connect (OSTI)

    Loy, D.A.; Carpenter, J.P.; Myers, S.A. [Sandia National Labs., Albuquerque, NM (United States)] [and others

    1996-12-31

    Under acidic sol-gel polymerization conditions, 1,3-bis(triethoxysilyl)-propane 1 and 1,4-bis(triethoxysilyl)butane 2 were shown to preferentially form cyclic disilsesquioxanes 3 and 4 rather than the expected 1,3-propylene- and 1,4-butylene-bridged polysilsesquioxane gels. Formation of 3 and 4 is driven by a combination of an intramolecular cyclization to six and seven membered rings, and a pronounced reduction in reactivity under acidic conditions as a function of increasing degree of condensation. The stability of cyclic disilsesquioxanes was confirmed with the synthesis of 3 and 4 in gram quantities; the cyclic disilsesquioxanes react slowly to give tricyclic dimers containing a thermodynamically stable eight membered siloxane ring. Continued reactions were shown to perserve the cyclic structure, opening up the possibility of utilizing cyclic disilsesquioxanes as sol-gel monomers. Preliminary polymerization studies with these new, carbohydrate-like monomers revealed the formation of network poly(cyclic disilsesquioxanes) under acidic conditions and polymerization with ring-opening under basic conditions.

  16. Mental Representations Formed From Educational Website Formats

    SciTech Connect (OSTI)

    Elizabeth T. Cady; Kimberly R. Raddatz; Tuan Q. Tran; Bernardo de la Garza; Peter D. Elgin

    2006-10-01

    The increasing popularity of web-based distance education places high demand on distance educators to format web pages to facilitate learning. However, limited guidelines exist regarding appropriate writing styles for web-based distance education. This study investigated the effect of four different writing styles on reader’s mental representation of hypertext. Participants studied hypertext written in one of four web-writing styles (e.g., concise, scannable, objective, and combined) and were then administered a cued association task intended to measure their mental representations of the hypertext. It is hypothesized that the scannable and combined styles will bias readers to scan rather than elaborately read, which may result in less dense mental representations (as identified through Pathfinder analysis) relative to the objective and concise writing styles. Further, the use of more descriptors in the objective writing style will lead to better integration of ideas and more dense mental representations than the concise writing style.

  17. On conduction, cooling flows and galaxy formation

    E-Print Network [OSTI]

    Fabian, A C; Morris, R G

    2002-01-01

    On the basis of the universal gas fraction in clusters of galaxies, we estimate that the effective thermal conductivity required to balance radiative cooling in the cores, where the gas temperature is 3-10keV, is about one tenth of the Spitzer rate. This confirms that thermal conduction can be important for the energy balance provided that it is not highly suppressed by magnetic fields in the gas. We determine the global effective conductivity in a sample of 29 clusters using published X-ray data on the inferred cooling rates and show that most lie between one and one tenth of the Spitzer rate. More work on the profiles in cooling flow clusters is required to test the conduction hypothesis further. We examine the possibility that conduction operates during galaxy formation, and show that it provides a simple explanation for the upper-mass cutoff in galaxy masses.

  18. On conduction, cooling flows and galaxy formation

    E-Print Network [OSTI]

    A. C. Fabian; L. M. Voigt; R. G. Morris

    2002-06-25

    On the basis of the universal gas fraction in clusters of galaxies, we estimate that the effective thermal conductivity required to balance radiative cooling in the cores, where the gas temperature is 3-10keV, is about one tenth of the Spitzer rate. This confirms that thermal conduction can be important for the energy balance provided that it is not highly suppressed by magnetic fields in the gas. We determine the global effective conductivity in a sample of 29 clusters using published X-ray data on the inferred cooling rates and show that most lie between one and one tenth of the Spitzer rate. More work on the profiles in cooling flow clusters is required to test the conduction hypothesis further. We examine the possibility that conduction operates during galaxy formation, and show that it provides a simple explanation for the upper-mass cutoff in galaxy masses.

  19. Abundance ratios in hierarchical galaxy formation

    E-Print Network [OSTI]

    D. Thomas

    1999-01-18

    The chemical enrichment and stellar abundance ratios of galaxies which form in a hierarchical clustering scheme are calculated. For this purpose I adopt the star formation histories (SFH) as they are delivered by semi-analytic models in Kauffmann (1996}. It turns out that the average SFH of cluster ellipticals does not yield globally alpha-enhanced stellar populations. The star burst that occurs when the elliptical forms in the major merger plays therefore a crucial role in producing alpha-enhancement. Only under the assumption that the IMF is significantly flattened with respect to the Salpeter value during the burst, a Mg/Fe overabundant population can be obtained. In particular for the interpretation of radial gradients in metallicity and alpha-enhancement, the mixing of global and burst populations are of great importance. The model predicts bright field galaxies to be less alpha-enhanced than their counterparts in clusters.

  20. Formation of nanofilament field emission devices

    DOE Patents [OSTI]

    Morse, Jeffrey D. (Martinez, CA); Contolini, Robert J. (Lake Oswego, OR); Musket, Ronald G. (Danville, CA); Bernhardt, Anthony F. (Berkeley, CA)

    2000-01-01

    A process for fabricating a nanofilament field emission device. The process enables the formation of high aspect ratio, electroplated nanofilament structure devices for field emission displays wherein a via is formed in a dielectric layer and is self-aligned to a via in the gate metal structure on top of the dielectric layer. The desired diameter of the via in the dielectric layer is on the order of 50-200 nm, with an aspect ratio of 5-10. In one embodiment, after forming the via in the dielectric layer, the gate metal is passivated, after which a plating enhancement layer is deposited in the bottom of the via, where necessary. The nanofilament is then electroplated in the via, followed by removal of the gate passification layer, etch back of the dielectric, and sharpening of the nanofilament. A hard mask layer may be deposited on top of the gate metal and removed following electroplating of the nanofilament.

  1. Fibrillar dimer formation of islet amyloid polypeptides

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Chiu, Chi -cheng; de Pablo, Juan J.

    2015-05-08

    Amyloid deposits of human islet amyloid polypeptide (hIAPP), a 37-residue hormone co-produced with insulin, have been implicated in the development of type 2 diabetes. Residues 20 – 29 of hIAPP have been proposed to constitute the amyloidogenic core for the aggregation process, yet the segment is mostly unstructured in the mature fibril, according to solid-state NMR data. Here we use molecular simulations combined with bias-exchange metadynamics to characterize the conformational free energies of hIAPP fibrillar dimer and its derivative, pramlintide. We show that residues 20 – 29 are involved in an intermediate that exhibits transient ?-sheets, consistent with recent experimentalmore »and simulation results. By comparing the aggregation of hIAPP and pramlintide, we illustrate the effects of proline residues on inhibition of the dimerization of IAPP. The mechanistic insights presented here could be useful for development of therapeutic inhibitors of hIAPP amyloid formation.« less

  2. Star-Formation Knots in IRAS Galaxies

    E-Print Network [OSTI]

    J. B. Hutchings

    1995-11-08

    Images of IRAS galaxies with a range of IR properties are examined for bright knots, both within and outside the galaxy. These are found almost exclusively in galaxies with steep IR spectra, but over a wide range of IR luminosity, and usually without strong nuclear activity. In most cases, the knots are likely to be star-formation induced by tidal interactions, and are seen in the early stages of such interactions. Detailed photometry is presented of knots in six representative galaxies. The knots appear to have a wide range of colour and luminosity, but it is argued that many are heavily reddened. Knots formed outside the parent galaxy may be a new generation of what later become globular clusters, but they appear to have a wide range of luminosities.

  3. Recombination energy in double white dwarf formation

    E-Print Network [OSTI]

    Nandez, Jose L A; Lombardi, James C

    2015-01-01

    In this Letter we investigate the role of recombination energy during a common envelope event. We confirm that taking this energy into account helps to avoid the formation of the circumbinary envelope commonly found in previous studies. For the first time, we can model a complete common envelope event, with a clean compact double white dwarf binary system formed at the end. The resulting binary orbit is almost perfectly circular. In addition to considering recombination energy, we also show that between 1/4 and 1/2 of the released orbital energy is taken away by the ejected material. We apply this new method to the case of the double-white dwarf system WD 1101+364, and we find that the progenitor system at the start of the common envelope event consisted of a $\\sim1.5M_\\odot$ red giant star in a $\\sim 30$ day orbit with a white dwarf companion.

  4. JET FORMATION IN COUNTERSTREAMING COLLISIONLESS PLASMAS

    SciTech Connect (OSTI)

    Kuramitsu, Y.; Sakawa, Y.; Takabe, H. [Institute of Laser Engineering, Osaka University, 2-6 Yamadaoka, Suita, Osaka 565-0871 (Japan); Waugh, J. N.; Woolsey, N. [Department of Physics, University of York, York, YO10 5DD (United Kingdom); Gregory, C. D.; Koenig, M. [Laboratoire pour l'Utilisation des Lasers Intenses, UMR 7605, CNRS, CEA, Universite Paris VI, Ecole Polytechnique, 91128 Palaiseau Cedex (France); Morita, T.; Aoki, H. [Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka, Osaka 560-0043 (Japan); Dono, S.; Tanji, H. [Graduate School of Engineering, Osaka University, 2-1, Yamadaoka, Suita, Osaka 565-0871 (Japan); Loupias, B., E-mail: kuramitsu-y@ile.osaka-u.ac.j [CEA, DAM, DIF, F-91297 Arpajon (France)

    2009-12-20

    Plasma jet formation was observed in counterstreaming plasmas in a laboratory experiment. In order to model an ambient plasma of astrophysical jets, the counterstreaming plasmas were created by irradiating a double CH-plane target with a high-power laser system. Since the mean free paths of the ions in terms of the counterstreaming motion were larger than the scale length of the experiment, the two-stream interaction of the plasmas was essentially collisionless. The time evolution of the jet collimation was obtained over several shots with different timing by shadowgraphy. When a single CH-plane target was irradiated, no jet collimation was observed. The counterstreaming plasma as an ambient plasma is essential for the jet plasma to collimate.

  5. Understanding galaxy formation with ISO deep surveys

    E-Print Network [OSTI]

    David Elbaz

    2005-03-17

    We present the results obtained through the various ISO extragalactic deep surveys. While IRAS revealed the existence of galaxies forming stars at a rate of a few tens (LIRGs) or even hundreds (ULIRGs) solar masses in the local universe, ISO not only discovered that these galaxies were already in place at redshift one, but also that they are not the extreme objects that we once believed them to be. Instead they appear to play a dominant role in shaping present-day galaxies as reflected by their role in the cosmic history of star formation and in producing the cosmic infrared background detected by the COBE satellite in the far infrared to sub-millimeter range.

  6. Observations of solute effects on bubble formation

    SciTech Connect (OSTI)

    Hofmeier, U.; Yaminsky, V.V.; Christenson, H.K.

    1995-09-01

    The authors have studied the effects of solute, in particular aqueous electrolyte, on bubble formation at capillary orifices and frits at varying gas flow rates. Using a stroboscope, video microscope, and rotating mirror, they have obtained pictures which show how bubble formation involves the interaction of bubbles at the orifice. These interactions depend on the value of the surface elasticity E due to positively (ethanol) or negatively (NaCl) adsorbed solute. At low flow rates consecutive bubbles do not interact. Each bubble detaches and leaves the orifice region before the next one starts forming. A intermediate flow rates the more closely spaced, consecutive bubbles begin to interact. In pure liquids there is no barrier to bubble coalescence and the detached bubble is fed by the subsequent bubble as this starts to grow. The process may be repeated several times before the original bubble has risen out of range. In solutions where E is large enough bubble coalescence is inhibited. Instead of feeding into the detached bubble the following bubble pushes it aside, and the bubbles appear to bounce off each other. Bouncing may give rise to a characteristic sequence of larger and smaller bubbles if the emerging bubbles break off prematurely from the orifice due to the inertia of the original bubble. The transition from feeding to bouncing depends critically on E of the solution and leads to a smaller average bubble size for large E values. At high flow rates detached bubbles are invariably fed by several subsequent ones. At very high flow rates the bubbling becomes chaotic, but the interaction of bubbles after leaving the orifice area produces smaller bubbles in solutions. Bouncing is more likely to occur with narrow and irregular capillaries. The dramatically different appearance of gas-sparged columns in salt water and freshwater has its origin in the difference between assemblies of pores showing mainly feeding (freshwater) or bouncing (salt water).

  7. Gas flows, star formation and galaxy evolution

    E-Print Network [OSTI]

    John E. Beckman; Emilio Casuso; Almudena Zurita; Monica Relaño

    2004-05-31

    In the first part of this article we show how observations of the chemical evolution of the Galaxy: G- and K-dwarf numbers as functions of metallicity, and abundances of the light elements, D, Li, Be and B, in both stars and the interstellar medium (ISM), lead to the conclusion that metal poor HI gas has been accreting to the Galactic disc during the whole of its lifetime, and is accreting today at a measurable rate, ~2 Msun per year across the full disc. Estimates of the local star formation rate (SFR) using methods based on stellar activity, support this picture. The best fits to all these data are for models where the accretion rate is constant, or slowly rising with epoch. We explain here how this conclusion, for a galaxy in a small bound group, is not in conflict with graphs such as the Madau plot, which show that the universal SFR has declined steadily from z=1 to the present day. We also show that a model in which disc galaxies in general evolve by accreting major clouds of low metallicity gas from their surroundings can explain many observations, notably that the SFR for whole galaxies tends to show obvious variability, and fractionally more for early than for late types, and yields lower dark to baryonic matter ratios for large disc galaxies than for dwarfs. In the second part of the article we use NGC 1530 as a template object, showing from Fabry-Perot observations of its Halpha emission how strong shear in this strongly barred galaxy acts to inhibit star formation, while compression acts to stimulate it.

  8. SUPPRESSION OF STAR FORMATION IN NGC 1266

    SciTech Connect (OSTI)

    Alatalo, Katherine; Lanz, Lauranne; Bitsakis, Theodoros; Appleton, Philip N.; Ogle, Patrick M.; Lacy, Mark; Lonsdale, Carol J.; Nyland, Kristina; Meier, David S.; Cales, Sabrina L.; Chang, Philip; Davis, Timothy A.; De Zeeuw, P. T.; Martín, Sergio

    2015-01-01

    NGC 1266 is a nearby lenticular galaxy that harbors a massive outflow of molecular gas powered by the mechanical energy of an active galactic nucleus (AGN). It has been speculated that such outflows hinder star formation (SF) in their host galaxies, providing a form of feedback to the process of galaxy formation. Previous studies, however, indicated that only jets from extremely rare, high-power quasars or radio galaxies could impart significant feedback on their hosts. Here we present detailed observations of the gas and dust continuum of NGC 1266 at millimeter wavelengths. Our observations show that molecular gas is being driven out of the nuclear region at M-dot {sub out}?110 M{sub ?} yr{sup –1}, of which the vast majority cannot escape the nucleus. Only 2 M {sub ?} yr{sup –1} is actually capable of escaping the galaxy. Most of the molecular gas that remains is very inefficient at forming stars. The far-infrared emission is dominated by an ultra-compact (? 50 pc) source that could either be powered by an AGN or by an ultra-compact starburst. The ratio of the SF surface density (?{sub SFR}) to the gas surface density (?{sub H{sub 2}}) indicates that SF is suppressed by a factor of ?50 compared to normal star-forming galaxies if all gas is forming stars, and ?150 for the outskirt (98%) dense molecular gas if the central region is powered by an ultra-compact starburst. The AGN-driven bulk outflow could account for this extreme suppression by hindering the fragmentation and gravitational collapse necessary to form stars through a process of turbulent injection. This result suggests that even relatively common, low-power AGNs are able to alter the evolution of their host galaxies as their black holes grow onto the M-? relation.

  9. Star formation and cosmic massive black hole formation, a universal process organized by angular momenta

    SciTech Connect (OSTI)

    Colgate, S. A.

    2004-01-01

    It is suggested that star formation is organized following the same principles as we have applied in a recent explanation of galaxy and massive black hole formation. In this scenario angular momentum is randomly distributed by tidal torquing among condensations, Lyman-{alpha} clouds or cores for star formation during the initial non-linear phase of collapse. This angular momentum is characterized by the parameter, {lambda}, the ratio of the angular momentum of the cloud to that of a Keplerian orbit with the same central mass and radius. This parameter is calculated in very many simulations of structure formation of the universe as well as core formation and appears to be universal and independent of any scale. The specific angular momentum during the collapse of every cloud is locally conserved and universally produces a near flat rotation curve M{sub formation of a flat rotation curve (protostellar) disk of mass M{sub dsk} {sup -}30 M{sub o} of radius R{sub dsk} {approx_equal} 1100 AU or 5.4 x 10{sup -3} pc. In such a disk {Sigma} {proportional_to} 1/R and reaches the RVI condition at R{sub crit} {approx_equal} 40 AU where M{sub

  10. STAR FORMATION AROUND SUPERGIANT SHELLS IN THE LARGE MAGELLANIC CLOUD

    SciTech Connect (OSTI)

    Book, Laura G.; Chu Youhua; Gruendl, Robert A.; Fukui, Yasuo

    2009-03-15

    We examine the recent star formation associated with four supergiant shells in the Large Magellanic Cloud (LMC): LMC 1, 4, 5, and 6, which have been shown to have simple expanding-shell structures. H II regions and OB associations are used to infer star formation in the last few Myr, while massive young stellar objects reveal the current ongoing star formation. Distributions of ionized H I and molecular components of the interstellar gas are compared with the sites of recent and current star formation to determine whether triggering has taken place. We find that a great majority of the current star formation has occurred in gravitationally unstable regions, and that evidence of triggered star formation is prevalent at both large and local scales.

  11. Cogeneration systems and processes for treating hydrocarbon containing formations

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Fowler, Thomas David (Houston, TX); Karanikas, John Michael (Houston, TX)

    2009-12-29

    A system for treating a hydrocarbon containing formation includes a steam and electricity cogeneration facility. At least one injection well is located in a first portion of the formation. The injection well provides steam from the steam and electricity cogeneration facility to the first portion of the formation. At least one production well is located in the first portion of the formation. The production well in the first portion produces first hydrocarbons. At least one electrical heater is located in a second portion of the formation. At least one of the electrical heaters is powered by electricity from the steam and electricity cogeneration facility. At least one production well is located in the second portion of the formation. The production well in the second portion produces second hydrocarbons. The steam and electricity cogeneration facility uses the first hydrocarbons and/or the second hydrocarbons to generate electricity.

  12. Method and apparatus for vibrating a substrate during material formation

    DOE Patents [OSTI]

    Bailey, Jeffrey A. (Richland, WA) [Richland, WA; Roger, Johnson N. (Richland, WA) [Richland, WA; John, Munley T. (Benton City, WA) [Benton City, WA; Walter, Park R. (Benton City, WA) [Benton City, WA

    2008-10-21

    A method and apparatus for affecting the properties of a material include vibrating the material during its formation (i.e., "surface sifting"). The method includes the steps of providing a material formation device and applying a plurality of vibrations to the material during formation, which vibrations are oscillations having dissimilar, non-harmonic frequencies and at least two different directions. The apparatus includes a plurality of vibration sources that impart vibrations to the material.

  13. Irregular spacing of heat sources for treating hydrocarbon containing formations

    SciTech Connect (OSTI)

    Miller, David Scott; Uwechue, Uzo Philip

    2012-06-12

    A method for treating a hydrocarbon containing formation includes providing heat input to a first section of the formation from one or more heat sources located in the first section. Fluids are produced from the first section through a production well located at or near the center of the first section. The heat sources are configured such that the average heat input per volume of formation in the first section increases with distance from the production well.

  14. The Formation and Destruction of Molecular Clouds and Galactic Star Formation

    E-Print Network [OSTI]

    Inutsuka, Shu-ichiro; Iwasaki, Kazunari; Hosokawa, Takashi

    2015-01-01

    We describe an overall picture of galactic-scale star formation. Recent high-resolution magneto-hydrodynamical simulations of two-fluid dynamics with cooling/heating and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a scenario in which molecular clouds form in interacting shells or bubbles on a galactic scale. First we estimate the ensemble-averaged growth rate of molecular clouds over a timescale larger than a million years. Next we perform radiation hydrodynamics simulations to evaluate the destruction rate of magnetized molecular clouds by the stellar FUV radiation. We also investigate the resultant star formation efficiency within a cloud which amounts to a low value (a few percent) if we adopt the power-law exponent -2.5 for the mass distribution of stars in the cloud. We finally describe the time evolution of the mass function of molecular clouds over a long timescale (>1Myr) and discuss the st...

  15. (U) modulator to provide a continuous stepped frequency signal format

    DOE Patents [OSTI]

    Walters, Glenn A. (Escondido, CA)

    1991-01-01

    A modulator provides a continuous signal format composed of discrete freqcy steps and is designed to eliminate frequency overlap or smearing normally associated with filter ringing.

  16. The modelling of feedback in star formation simulations

    E-Print Network [OSTI]

    Dale, James E

    2015-01-01

    I review the current state of numerical simulations of stellar feedback in the context of star formation at scales ranging from the formation of individual stars to models of galaxy formation including cosmic reionisation. I survey the wealth of algorithms developed recently to solve the radiative transfer problem and to simulate stellar winds, supernovae and protostellar jets. I discuss the results of these simulations with regard to star formation in molecular clouds, the interaction of different feedback mechanisms with each other and with magnetic fields, and in the wider context of galactic-- and cosmological--scale simulations.

  17. Microbial-mediated method for metal oxide nanoparticle formation...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Search Title: Microbial-mediated method for metal oxide nanoparticle formation The invention is directed to a method for producing metal oxide nanoparticles, the method...

  18. Room-temperature Formation of Hollow Cu2O Nanoparticles

    E-Print Network [OSTI]

    Hung, Ling-I

    2011-01-01

    is prohibited by the surface oxide layer, the thickness ofthe formation of an oxide layer prevents further exposure ofpenetrating into the oxide layer rapidly by tunneling to

  19. Accounting for Variation of Diminutive Formation in Porteño Spanish

    E-Print Network [OSTI]

    Norrmann-Vigil, Ingrid

    2012-01-01

    Accounting for Variation of Diminutive Formation in Porteñobase, the inclusion Accounting for Variation of Diminutiveas additive, thus accounting for cumulativity effects” (2).

  20. COLD BUBBLE FORMATION DURING TOKAMAK DENSITY LIMIT DISRUPTIONS

    E-Print Network [OSTI]

    Howard, John

    COLD BUBBLE FORMATION DURING TOKAMAK DENSITY LIMIT DISRUPTIONS J. HOWARD, M. PERSSON* Plasma Research Laboratory, Research School of Physical Sciences, Australian National University, Canberra

  1. Method for determining formation quality factor from well log...

    Office of Scientific and Technical Information (OSTI)

    determining formation quality factor from well log data and its application to seismic reservoir characterization Citation Details In-Document Search Title: Method for...

  2. "A New Paradigm for Secondary Eyewall Formation in Tropical Cyclones...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Road Princeton, NJ 08540-6649 "A New Paradigm for Secondary Eyewall Formation in Tropical Cyclones", Chun-Chieh Wu (National Taiwan University) Contact Information Website: Website...

  3. Chemistry & Biology Aryl-aldehyde Formation in Fungal Polyketides

    E-Print Network [OSTI]

    Zhao, Huimin

    Chemistry & Biology Article Aryl-aldehyde Formation in Fungal Polyketides: Discovery at Urbana-Champaign, Urbana, IL 61801, USA 2Department of Chemistry, University of Illinois at Urbana

  4. Histamine Formation and Honeycombing During Decomposition of Skipjack Tuna,

    E-Print Network [OSTI]

    Histamine Formation and Honeycombing During Decomposition of Skipjack Tuna, Katsuwonus pelamis pelamis, caught in Hawaiian waters. Fresh skipjack tuna tis- sue was practically devoid of histamine

  5. Lyalpha EMITTERS IN HIERARCHICAL GALAXY FORMATION. II. ULTRAVIOLET...

    Office of Scientific and Technical Information (OSTI)

    Lyalpha EMITTERS IN HIERARCHICAL GALAXY FORMATION. II. ULTRAVIOLET CONTINUUM LUMINOSITY FUNCTION AND EQUIVALENT WIDTH DISTRIBUTION Citation Details In-Document Search Title:...

  6. Formation and retention of methane in coal

    SciTech Connect (OSTI)

    Hucka, V.J.; Bodily, D.M.; Huang, H.

    1992-05-15

    The formation and retention of methane in coalbeds was studied for ten Utah coal samples, one Colorado coal sample and eight coal samples from the Argonne Premium Coal Sample Bank.Methane gas content of the Utah and Colorado coals varied from zero to 9 cm{sup 3}/g. The Utah coals were all high volatile bituminous coals. The Colorado coal was a gassy medium volatile bituminous coal. The Argonne coals cover a range or rank from lignite to low volatile bituminous coal and were used to determine the effect of rank in laboratory studies. The methane content of six selected Utah coal seams and the Colorado coal seam was measured in situ using a special sample collection device and a bubble desorbometer. Coal samples were collected at each measurement site for laboratory analysis. The cleat and joint system was evaluated for the coal and surrounding rocks and geological conditions were noted. Permeability measurements were performed on selected samples and all samples were analyzed for proximate and ultimate analysis, petrographic analysis, {sup 13}C NMR dipolar-dephasing spectroscopy, and density analysis. The observed methane adsorption behavior was correlated with the chemical structure and physical properties of the coals.

  7. Halo Formation in Warm Dark Matter Models

    E-Print Network [OSTI]

    Paul Bode; Jeremiah P. Ostriker; Neil Turok

    2001-05-29

    Discrepancies have emerged between the predictions of standard cold dark matter (CDM) theory and observations of clustering on sub-galactic scales. Warm dark matter (WDM) is a simple modification of CDM in which the dark matter particles have initial velocities due either to their having decoupled as thermal relics, or having been formed via non-equilibrium decay. We investigate the nonlinear gravitational clustering of WDM with a high resolution N-body code, and identify a number of distinctive observational signatures. Relative to CDM, halo concentrations and core densities are lowered, core radii are increased, and large halos emerge with far fewer low mass satellites. The number of small halos is suppressed, and those present are formed by `top down' fragmentation of caustics, as part of a `cosmic web' connecting massive halos. Few small halos form outside this web. If we identify small halos with dwarf galaxies, their number, spatial distribution, and formation epoch appear in better agreement with the observations for WDM than they are for CDM.

  8. Star formation and substructure in galaxy clusters

    SciTech Connect (OSTI)

    Cohen, Seth A.; Hickox, Ryan C.; Wegner, Gary A.; Einasto, Maret; Vennik, Jaan

    2014-03-10

    We investigate the relationship between star formation (SF) and substructure in a sample of 107 nearby galaxy clusters using data from the Sloan Digital Sky Survey. Several past studies of individual galaxy clusters have suggested that cluster mergers enhance cluster SF, while others find no such relationship. The SF fraction in multi-component clusters (0.228 ± 0.007) is higher than that in single-component clusters (0.175 ± 0.016) for galaxies with M{sub r}{sup 0.1}

  9. Constructing Hydraulic Barriers in Deep Geologic Formations

    SciTech Connect (OSTI)

    Carter, E.E.; Carter, P.E. [Technologies Co, Texas (United States); Cooper, D.C. [Ph.D. Idaho National Laboratory, Idaho Falls, ID (United States)

    2008-07-01

    Many construction methods have been developed to create hydraulic barriers to depths of 30 to 50 meters, but few have been proposed for depths on the order of 500 meters. For these deep hydraulic barriers, most methods are potentially feasible for soil but not for hard rock. In the course of researching methods of isolating large subterranean blocks of oil shale, the authors have developed a wax thermal permeation method for constructing hydraulic barriers in rock to depths of over 500 meters in competent or even fractured rock as well as soil. The technology is similar to freeze wall methods, but produces a permanent barrier; and is potentially applicable in both dry and water saturated formations. Like freeze wall barriers, the wax thermal permeation method utilizes a large number of vertical or horizontal boreholes around the perimeter to be contained. However, instead of cooling the boreholes, they are heated. After heating these boreholes, a specially formulated molten wax based grout is pumped into the boreholes where it seals fractures and also permeates radially outward to form a series of columns of wax-impregnated rock. Rows of overlapping columns can then form a durable hydraulic barrier. These barriers can also be angled above a geologic repository to help prevent influx of water due to atypical rainfall events. Applications of the technique to constructing containment structures around existing shallow waste burial sites and water shutoff for mining are also described. (authors)

  10. Transient Pulse Formation in Jasmonate Signaling Pathway

    E-Print Network [OSTI]

    Subhasis Banerjee; Indrani Bose

    2010-03-03

    The jasmonate (JA) signaling pathway in plants is activated as defense response to a number of stresses like attacks by pests or pathogens and wounding by animals. Some recent experiments provide significant new knowledge on the molecular detail and connectivity of the pathway. The pathway has two major components in the form of feedback loops, one negative and the other positive. We construct a minimal mathematical model, incorporating the feedback loops, to study the dynamics of the JA signaling pathway. The model exhibits transient gene expression activity in the form of JA pulses in agreement with experimental observations. The dependence of the pulse amplitude, duration and peak time on the key parameters of the model is determined computationally. The deterministic and stochastic aspects of the pathway dynamics are investigated using both the full mathematical model as well as a reduced version of it. We also compare the mechanism of pulse formation with the known mechanisms of pulse generation in some bacterial and viral systems.

  11. Modeling the formation of in vitro filopodia

    E-Print Network [OSTI]

    K. -C. Lee; A. Gopinathan; J. M. Schwarz

    2010-05-13

    Filopodia are bundles of actin filaments that extend out ahead of the leading edge of a crawling cell to probe its upcoming environment. {\\it In vitro} experiments [D. Vignjevic {\\it et al.}, J. Cell Biol. {\\bf 160}, 951 (2003)] have determined the minimal ingredients required for the formation of filopodia from the dendritic-like morphology of the leading edge. We model these experiments using kinetic aggregation equations for the density of growing bundle tips. In mean field, we determine the bundle size distribution to be broad for bundle sizes smaller than a characteristic bundle size above which the distribution decays exponentially. Two-dimensional simulations incorporating both bundling and cross-linking measure a bundle size distribution that agrees qualitatively with mean field. The simulations also demonstrate a nonmonotonicity in the radial extent of the dendritic region as a function of capping protein concentration, as was observed in experiments, due to the interplay between percolation and the ratcheting of growing filaments off a spherical obstacle.

  12. Surface coating for prevention of crust formation

    DOE Patents [OSTI]

    Kronberg, James W. (Aiken, SC)

    1994-01-01

    A flexible surface coating which promotes the removal of deposits as they reach the surface by preventing adhesion and crust formation. Flexible layers are attached to each side of a flexible mesh substrate comprising of a plurality of zones composed of one or more neighboring cells, each zone having a different compressibility than its adjacent zones. The substrate is composed of a mesh made of strands and open cells. The cells may be filled with foam. Studs or bearings may also be positioned in the cells to increase the variation in compressibility and thus the degree of flexing of the coating. Surface loading produces varying amounts of compression from point to point causing the coating to flex as deposits reach it, breaking up any hardening deposits before a continuous crust forms. Preferably one or more additional layers are also used, such as an outer layer of a non-stick material such as TEFLON, which may be pigmented, and an inner, adhesive layer to facilitate applying the coating to a surface.

  13. Explaining the formation of bulges with MOND

    E-Print Network [OSTI]

    Combes, F

    2015-01-01

    In the cold dark matter (CDM) paradigm, bulges easily form through galaxy mergers, either major or minor, or through clumpy disks in the early universe, where clumps are driven to the center by dynamical friction. Also pseudo-bulges, with a more disky morphology and kinematics, can form more slowly through secular evolution of a bar, where resonant stars are elevated out of the plane, in a peanut/box shape. As a result, in CDM cosmological simulations, it is very difficult to find a bulgeless galaxy, while they are observed very frequently in the local universe. A different picture emerges in alternative models of the missing mass problem. In MOND (MOdified Newtonian Dynamics), galaxy mergers are much less frequent, since the absence of dark matter halos reduces the dynamical friction between two galaxies. Also, while clumpy galaxies lead to rapid classical bulge formation in CDM, the inefficient dynamical friction with MOND in the early-universe galaxies prevents the clumps to coalesce together in the center...

  14. Porosity reduction in Monterey Formation, California

    SciTech Connect (OSTI)

    Compton, J.S.

    1987-05-01

    Porosity and grain density were determined for different lithologies from throughout a 1.2-km thick section of the Monterey and Sisquoc formations in the Santa Maria basin area, California. Porosity reduction by physical and chemical compaction in the predominantly siliceous sediment is controlled largely by the bulk sediment composition and silica phase transformations. Physical compaction of sediment grains from increasing overburden pressure is responsible for most of the gradual porosity reduction with increasing burial depth in opal-A siliceous ooze and diatomite. The porous, incompressible diatom frustule maintains a high porosity relative to clayey and calcareous sediment. Therefore, a positive correlation exists between porosity and biogenic silica (diatom) content of the sediment. During the opal-A to opal-CT silica phase transformation, solution of the porous diatom frustule and precipitation of cryptocrystalline opal-CT results in a porosity reduction that roughly correlates with the biogenic silica content of the sediment. Local porosity reduction occurs in pore-filling dolomite and chert nodules. Dry bulk density as well as porosity reduction tend to increase with sediment depth. Dolomite and organic matter have the most significant influence on the bulk density because of their respective high and low density. The maximum burial depth of the uplifted and eroded section is estimated by overlapping the porosity-depth relation of average deep-sea siliceous ooze.

  15. Essays on Dynamic Value Change Perspective in Resource Based View, Determinants of Alliance Formation and Risk Preference in Alliance Formation 

    E-Print Network [OSTI]

    Jun, Ik Su

    2011-02-22

    ON DYNAMIC VALUE CHANGE PERSPECTIVE IN RESOURCE BASED VIEW, DETERMINANTS OF ALLIANCE FORMATION AND RISK PREFERENCE IN ALLIANCE FORMATION A Dissertation by IK SU JUN Submitted to the Office of Graduate Studies of Texas A&M University... in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY December 2009 Major Subject: Agricultural Economics ESSAYS ON DYNAMIC VALUE CHANGE PERSPECTIVE IN RESOURCE BASED VIEW, DETERMINANTS OF ALLIANCE FORMATION...

  16. Academic Registry Guidelines on Submission and Format of Thesis

    E-Print Network [OSTI]

    Greenaway, Alan

    Academic Registry Guidelines on Submission and Format of Thesis Please check with Academic Registry before submitting a thesis as the following Regulations may be subject to change from time to time. The following is a statement of the provisions governing the submission and format of a thesis. These provisions

  17. Video Digests: A Browsable, Skimmable Format for Informational Lecture Videos

    E-Print Network [OSTI]

    O'Brien, James F.

    Video Digests: A Browsable, Skimmable Format for Informational Lecture Videos Amy Pavel, Colorado- ing current timeline-based video players. Video digests are a new format for informational videos authors create such digests using transcript-based interactions. With our tools, authors can manually

  18. Self-Stabilizing Robot Formations over Unreliable Networks

    E-Print Network [OSTI]

    Liberzon, Daniel

    -stabilization ensures that the robots can adapt to changes in the desired target formation. Categories and Subject17 Self-Stabilizing Robot Formations over Unreliable Networks SETH GILBERT Ecole Polytechnique F Descriptors: F.1.2 [Computation by Abstract Devices]: Modes of Compu- tation--Interactive and reactive

  19. Time Series Photometry Data: Standard Access, Standard Formats

    E-Print Network [OSTI]

    Holl, András

    Time Series Photometry Data: Standard Access, Standard Formats Andr#19; as Holl Konkoly Observatory a discussion on data access and #12;le format aspects of photometry. Introduction Presently there is time series photometry data available in public databases, but the access to these varies from one collection

  20. Ring current formation influenced by solar wind substorm conditions

    E-Print Network [OSTI]

    Winglee, Robert M.

    Click Here for Full Article Ring current formation influenced by solar wind substorm conditions M outflows during an internally driven substorm. We show that the energization of the ions is not correlated with the time that the ions leave the ionosphere; instead energization is correlated with the formation

  1. Dictyostelium Myosin Bipolar Thick Filament Formation: Importance of Charge

    E-Print Network [OSTI]

    Spudich, James A.

    Dictyostelium Myosin Bipolar Thick Filament Formation: Importance of Charge and Specific Domains and Molecular Biology, Northwestern University, Chicago, Illinois, United States of America, 3 UNC of America Myosin-II thick filament formation in Dictyostelium is an excellent system for investigating

  2. Amyloid Oligomer Formation Probed by Water Proton Magnetic Resonance Spectroscopy

    E-Print Network [OSTI]

    Berry, R. Stephen

    Amyloid Oligomer Formation Probed by Water Proton Magnetic Resonance Spectroscopy J. H. Walton, R, Chicago, Illinois; and § Department of Pharmacology, University of California, Davis, California ABSTRACT Formation of amyloid oligomers, the most toxic species of amyloids in degenerative diseases, is critically

  3. Laboratory Simulations of Molecular Hydrogen Formation in the Early Universe

    E-Print Network [OSTI]

    Savin, Daniel Wolf

    Laboratory Simulations of Molecular Hydrogen Formation in the Early Universe: A Progress Report D Heidelberg, Germany Department of Chemistry, University of Illinois, 600 South Mathews Avenue, Urbana, Il-la-Neuve B-1348, Belgium Abstract. During the epoch of protogalaxy and first star formation, H2 is the main

  4. CONSTRAINING THE ENVIRONMENT OF CH FORMATION WITH CH

    E-Print Network [OSTI]

    Oka, Takeshi

    CONSTRAINING THE ENVIRONMENT OF CH + FORMATION WITH CH + 3 OBSERVATIONS This article has been reserved. Printed in the U.S.A. CONSTRAINING THE ENVIRONMENT OF CH+ FORMATION WITH CH+ 3 OBSERVATIONS Nick of Illinois at Urbana-Champaign, Urbana, IL 61801, USA 2 Department of Astronomy and Astrophysics

  5. Universality in dynamical formation of entanglement for quantum chaos

    SciTech Connect (OSTI)

    Kubotani, Hiroto; Toda, Mikito; Adachi, Satoshi [Institute of Physics, Faculty of Engineering, Kanagawa University, Yokohama 221-8686 (Japan); Department of Physics, Faculty of Science, Nara Women's University, Nara 630-8506 (Japan); Department of Physics, Faculty of Science, Tokyo Institute of Technology, Meguro 152-8550 (Japan)

    2006-09-15

    Dynamical formation of entanglement is studied for quantum chaotic biparticle systems. We find that statistical properties of the Schmidt eigenvalues for strong chaos are well described by the random matrix theory of the Laguerre unitary ensemble. This implies that entanglement formation for quantum chaos has universal properties, and does not depend on specific aspects of the systems.

  6. Formation and distribution of benzene on Titan V. Vuitton,1

    E-Print Network [OSTI]

    Yelle, Roger V.

    Formation and distribution of benzene on Titan V. Vuitton,1 R. V. Yelle,1 and J. Cui1 Received 29 a study of the formation and distribution of benzene (C6H6) on Titan. Analysis of the Cassini Mass Spectrometer (INMS) measurements of benzene densities on 12 Titan passes shows that the benzene signal exhibits

  7. UFO (UnFold Operator) default data format

    SciTech Connect (OSTI)

    Kissel, L.; Biggs, F. ); Marking, T.R. )

    1991-05-01

    The default format for the storage of x,y data for use with the UFO code is described. The format assumes that the data stored in a file is a matrix of values; two columns of this matrix are selected to define a function of the form y = f(x). This format is specifically designed to allow for easy importation of data obtained from other sources, or easy entry of data using a text editor, with a minimum of reformatting. This format is flexible and extensible through the use of inline directives stored in the optional header of the file. A special extension of the format implements encoded data which significantly reduces the storage required as compared wth the unencoded form. UFO supports several extensions to the file specification that implement execute-time operations, such as, transformation of the x and/or y values, selection of specific columns of the matrix for association with the x and y values, input of data directly from other formats (e.g., DAMP and PFF), and a simple type of library-structured file format. Several examples of the use of the format are given.

  8. Dissolved organic carbon export with North Pacific Intermediate Water formation

    E-Print Network [OSTI]

    Hansell, Dennis

    Dissolved organic carbon export with North Pacific Intermediate Water formation Dennis A. Hansell 2002. [1] An evaluation of DOC export with the formation of North Pacific Intermediate Water east of Japan. The new intermediate water, formed at a rate of 2­5 Sv, exports DOC at 13 ± 6 Tg DOC yr

  9. METHOD Open Access A standard variation file format for human

    E-Print Network [OSTI]

    Yandell, Mark

    was originally developed during the human genome project to compare human genome annotations [17]. ImportantlyMETHOD Open Access A standard variation file format for human genome sequences Martin G Reese1 data. The 10Gen dataset, ten human genomes in GVF format, is freely available for com- munity analysis

  10. Discrete mechanics, optimal control and formation flying spacecraft

    E-Print Network [OSTI]

    Patrick, George

    Discrete mechanics, optimal control and formation flying spacecraft Oliver Junge Center-Bl¨obaum partially supported by the CRC 376 Oliver Junge Discrete mechanics, optimal control and formation flying spacecraft p.1 #12;Outline mechanical optimal control problem direct discretization of the variational

  11. Hydrogen Peroxide Formation Rates in a PEMFC Anode and Cathode

    E-Print Network [OSTI]

    Sethuraman, Vijay A.

    Hydrogen Peroxide Formation Rates in a PEMFC Anode and Cathode Effect of Humidity and Temperature Hydrogen peroxide H2O2 formation rates in a proton exchange membrane fuel cell PEMFC anode and cathode were, has the capability to be the structural and fundamental unit of an impending hydrogen economy. Two

  12. Astronomy 241: Foundations of Astrophysics I 21. Solar System Formation

    E-Print Network [OSTI]

    Barnes, Joshua Edward

    to flow in. #12;Three-Trillion-Mile-Long Jet From a Wobbly Star #12;Planet Formation: The Frost Line The disk was hot at the center, and cool further out. Inside the frost line, only rocks & metals can of Mars and Jupiter -- roughly 4 AU from the Sun. #12;Planet Formation: Terrestrial Planets 1. Within

  13. Paleoecology and paleontology of the Lower Cretaceous Kiowa Formation, Kansas

    E-Print Network [OSTI]

    Scott, R. W.

    1970-01-15

    OF KANSAS PALEONTOLOGICAL CONTRIBUTIONS ARTICLE 52 (CRETACEOUS 1) PALEOECOLOGY AND PALEONTOLOGY OF THE LOWER CRETACEOUS KIOWA FORMATION, KANSAS ROBERT W. SCOTT Department of Geology, University of Kansas, Lawrence Present address: Waynesburg College... PALEOECOLOGY AND PALEONTOLOGY OF THE LOWER CRETACEOUS KIOWA FORMATION, KANSAS ROBERT W. SCOTT Department of Geology, University of Kansas, Lawrence Present address: Waynesburg College, Waynesburg, Pennsylvania CONTENTS PAGE ABSTRACT 5 Interspecific...

  14. MODELING OF POROSITY FORMATION AND FEEDING FLOW IN STEEL CASTING

    E-Print Network [OSTI]

    Beckermann, Christoph

    , or even larger shrinkage cavities found in inadequately fed cast sections. Microporosity can cause leaksMODELING OF POROSITY FORMATION AND FEEDING FLOW IN STEEL CASTING Kent D. Carlson, Zhiping Lin pressure, feeding flow, and porosity formation and growth in steel castings during solidification

  15. Microfluidics Formation of Bubbles in a Multisection Flow-Focusing

    E-Print Network [OSTI]

    Prentiss, Mara

    Microfluidics Formation of Bubbles in a Multisection Flow-Focusing Junction Michinao Hashimoto the stable formation of trains of mono-, bi-, and tri-disperse bubbles in microfluidic flow- focusing (FF-assembly through the patterns of flow created by the bubbles. 1.1 Bubbles and Droplets in Microfluidics

  16. Pattern formation in nonequilibrium physics J. P. Gollub

    E-Print Network [OSTI]

    Gollub, Jerry P.

    concepts to emerge in this century. At the center of our modern understanding of pattern formationPattern formation in nonequilibrium physics J. P. Gollub Haverford College, Haverford, Pennsylvania 19041 and Department of Physics, University of Pennsylvania, Philadelphia, Pennsylvania 19104 J. S

  17. CHARACTERIZATION OF COLLOIDS FROM HANFORD FORMATION SEDIMENTS REACTED WITH

    E-Print Network [OSTI]

    Flury, Markus

    CHARACTERIZATION OF COLLOIDS FROM HANFORD FORMATION SEDIMENTS REACTED WITH SIMULATED TANK WASTE with the Hanford sediments. I would like to extend my sincere appreciation to Professor Jim Henson, Dan Hardesty for me to have all of my work done. iv #12;CHARACTERIZATION OF COLLOIDS FROM HANFORD FORMATION SEDIMENTS

  18. Sequence Stratigraphy of the Glenshaw Formation (MiddleLate

    E-Print Network [OSTI]

    Martino, Ronald L.

    Sequence Stratigraphy of the Glenshaw Formation (Middle­Late Pennsylvanian) in the Central. L., 2004, Sequence stratigraphy of the Glenshaw Formation (middle­late Pennsylvanian) in the central Appalachian basin, in J. C. Pashin and R. A. Gastaldo, eds., Sequence stratigraphy, paleoclimate

  19. Finite Element Model of Fracture Formation on Growing Surfaces

    E-Print Network [OSTI]

    Prusinkiewicz, Przemyslaw

    Finite Element Model of Fracture Formation on Growing Surfaces Pavol Federl and Przemyslaw-mail: federl|pwp@cpsc.ucalgary.ca Abstract We present a model of fracture formation on surfaces of bilayered materials. The model makes it possible to synthesize patterns of fractures induced by growth or shrinkage

  20. Thickness-dependent secondary structure formation of tubelike polymers

    E-Print Network [OSTI]

    Janke, Wolfhard

    OFFPRINT Thickness-dependent secondary structure formation of tubelike polymers T. Vogel, T.epljournal.org doi: 10.1209/0295-5075/85/10003 Thickness-dependent secondary structure formation of tubelike polymers the conformational phase diagram of a simple model for flexible polymers with explicit thickness. The thickness

  1. Filaments in simulations of molecular cloud formation

    SciTech Connect (OSTI)

    Gómez, Gilberto C.; Vázquez-Semadeni, Enrique

    2014-08-20

    We report on the filaments that develop self-consistently in a new numerical simulation of cloud formation by colliding flows. As in previous studies, the forming cloud begins to undergo gravitational collapse because it rapidly acquires a mass much larger than the average Jeans mass. Thus, the collapse soon becomes nearly pressureless, proceeding along its shortest dimension first. This naturally produces filaments in the cloud and clumps within the filaments. The filaments are not in equilibrium at any time, but instead are long-lived flow features through which the gas flows from the cloud to the clumps. The filaments are long-lived because they accrete from their environment while simultaneously accreting onto the clumps within them; they are essentially the locus where the flow changes from accreting in two dimensions to accreting in one dimension. Moreover, the clumps also exhibit a hierarchical nature: the gas in a filament flows onto a main, central clump but other, smaller-scale clumps form along the infalling gas. Correspondingly, the velocity along the filament exhibits a hierarchy of jumps at the locations of the clumps. Two prominent filaments in the simulation have lengths ?15 pc and masses ?600 M {sub ?} above density n ? 10{sup 3} cm{sup –3} (?2 × 10{sup 3} M {sub ?} at n > 50 cm{sup –3}). The density profile exhibits a central flattened core of size ?0.3 pc and an envelope that decays as r {sup –2.5} in reasonable agreement with observations. Accretion onto the filament reaches a maximum linear density rate of ?30 M {sub ?} Myr{sup –1} pc{sup –1}.

  2. Solution mining systems and methods for treating hydrocarbon containing formations

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); de Rouffignac, Eric Pierre (Rijswijk, NL); Schoeling, Lanny Gene (Katy, TX)

    2009-07-14

    A method for treating an oil shale formation comprising nahcolite is disclosed. The method includes providing a first fluid to a portion of the formation through at least two injection wells. A second fluid is produced from the portion through at least one injection well until at least two injection wells are interconnected such that fluid can flow between the two injection wells. The second fluid includes at least some nahcolite dissolved in the first fluid. The first fluid is injected through one of the interconnected injection wells. The second fluid is produced from at least one of the interconnected injection wells. Heat is provided from one or more heaters to the formation to heat the formation. Hydrocarbon fluids are produced from the formation.

  3. HIERARCHICAL STRUCTURE FORMATION AND MODES OF STAR FORMATION IN HICKSON COMPACT GROUP 31

    SciTech Connect (OSTI)

    Gallagher, S. C. [Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7 (Canada); Durrell, P. R. [Department of Physics and Astronomy, Youngstown State University, Youngstown, OH 44555 (United States); Elmegreen, D. M. [Department of Physics and Astronomy, Vassar College, Poughkeepsie, NY 12604 (United States); Chandar, R. [Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390 (United States); English, J. [Department of Physics and Astronomy, University of Manitoba, Winnipeg, MN R3T 2N2 (Canada); Charlton, J. C.; Gronwall, C.; Young, J. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Tzanavaris, P.; Hornschemeier, A. E. [Laboratory for X-ray Astrophysics, NASA's Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Johnson, K. E. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States); Mendes de Oliveira, C. [Instituto de Astronomia, Geofisica, e Ciencias Atmosfericas da Universidade de Sao Paulo, Sao Paulo (Brazil); Whitmore, B.; Maybhate, Aparna [Space Telescope Science Institute, Baltimore, MD 21218-2463 (United States); Zabludoff, Ann [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)], E-mail: sgalla4@uwo.ca

    2010-02-15

    The handful of low-mass, late-type galaxies that comprise Hickson Compact Group 31 (HCG 31) is in the midst of complex, ongoing gravitational interactions, evocative of the process of hierarchical structure formation at higher redshifts. With sensitive, multicolor Hubble Space Telescope imaging, we characterize the large population of < 10 Myr old star clusters (SCs) that suffuse the system. From the colors and luminosities of the young SCs, we find that the galaxies in HCG 31 follow the same universal scaling relations as actively star-forming galaxies in the local universe despite the unusual compact group environment. Furthermore, the specific frequency of the globular cluster system is consistent with the low end of galaxies of comparable masses locally. This, combined with the large mass of neutral hydrogen and tight constraints on the amount of intragroup light, indicate that the group is undergoing its first epoch of interaction-induced star formation. In both the main galaxies and the tidal-dwarf candidate, F, stellar complexes, which are sensitive to the magnitude of disk turbulence, have both sizes and masses more characteristic of z = 1-2 galaxies. After subtracting the light from compact sources, we find no evidence for an underlying old stellar population in F-it appears to be a truly new structure. The low-velocity dispersion of the system components, available reservoir of H I, and current star formation rate of {approx}10 M {sub sun} yr{sup -1} indicate that HCG 31 is likely to both exhaust its cold gas supply and merge within {approx}1 Gyr. We conclude that the end product will be an isolated, X-ray-faint, low-mass elliptical.

  4. Solution mining dawsonite from hydrocarbon containing formations with a chelating agent

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX)

    2009-07-07

    A method for treating an oil shale formation comprising dawsonite includes providing heat from one or more heaters to the formation to heat the formation. Hydrocarbon fluids are produced from the formation. At least some dawsonite in the formation is decomposed with the provided heat. A chelating agent is provided to the formation to dissolve at least some dawsonite decomposition products. The dissolved dawsonite decomposition products are produced from the formation.

  5. Controlling formation fines at their sources to maintain well productivity

    SciTech Connect (OSTI)

    Nguyen, P.D.; Weaver, J.D.; Rickman, R.D.; Dusterhoft, R.G.; Parker, M.A.

    2007-05-15

    Migration of formation fines has been shown to cause production decline in many wells. Despite the availability of new downhole tools for use in well stimulation and completion, the ability to sustain desired production levels is often plagued with fines migration problems. The solution to this problem is appropriate treatment to mitigate fines migration at its source. This paper describes the use of an ultra-thin tackifying agent (UTTA) for stabilizing fines in high-rate producing or injection wells. This UTTA is applied as part of an initial prepad in fracturing or gravel-packing operations, as a remedial treatment, or as a post-treatment following acid fracturing or matrix acidizing treatments. The primary purpose of UTTA application is to immobilize formation fines so that they will not detach, migrate with flowing fluids, plug the pore channels, and reduce the flow path permeability. Results of laboratory testing indicate that the UTTA system is applicable to most types of formation fines, including coals, sandstones, and carbonates. Once injected into the formation matrix or proppant pack, the UTTA forms a thin film on formation surfaces, encapsulating the fines. Capillary action helps pull the tackifier into the contact points, fixing the particulate in place without plugging the pore throat. The UTTA does not require a shut-in time after its application. The thin film tackifier does not harden, but remains flexible, enhancing the ability of a formation to withstand stress cycling and allowing the formation to handle high shear stress during high flow rates.

  6. Sequestration of Dissolved CO2 in the Oriskany Formation

    SciTech Connect (OSTI)

    Dilmore, R.M.; Allen, D.E. (Salem State College, Salem, MA); McCarthy-Jones, J.R.; Hedges, S.W.; Soong, Yee

    2008-04-15

    Experiments were conducted to determine the solubility of CO2 in a natural brine solution of the Oriskany formation under elevated temperature and pressure conditions. These data were collected at temperatures of 22 and 75 °C and pressures between 100 and 450 bar. Experimentally determined data were compared with CO2 solubility predictions using a model developed by Duan and Sun (Chem. Geol. 2003, 193, 257-271). Model results compare well with Oriskany brine CO2 solubility data collected experimentally, suggesting that the Duan and Sun model is a reliable tool for estimating solution CO2 capacity in high salinity aquifers in the temperature and pressure range evaluated. The capacity for the Oriskany formation to sequester dissolved CO2 was calculated using results of the solubility models, estimation of the density of CO2 saturated brine, and available geographic information system (GIS) information on the formation depth and thickness. Results indicate that the Oriskany formation can hold approximately 0.36 gigatonnes of dissolved CO2 if the full basin is considered. When only the region where supercritical CO2 can exist (temperatures greater than 31° C and pressures greater than 74 bar) is considered, the capacity of the Oriskany formation to sequester dissolved CO2 is 0.31 gigatonnes. The capacity estimate considering the potential to sequester free-phase supercritical CO2 if brine were displaced from formation pore space is 8.8 gigatonnes in the Oriskany formation.

  7. Systems and methods for producing hydrocarbons from tar sands formations

    DOE Patents [OSTI]

    Li, Ruijian (Katy, TX); Karanikas, John Michael (Houston, TX)

    2009-07-21

    A system for treating a tar sands formation is disclosed. A plurality of heaters are located in the formation. The heaters include at least partially horizontal heating sections at least partially in a hydrocarbon layer of the formation. The heating sections are at least partially arranged in a pattern in the hydrocarbon layer. The heaters are configured to provide heat to the hydrocarbon layer. The provided heat creates a plurality of drainage paths for mobilized fluids. At least two of the drainage paths converge. A production well is located to collect and produce mobilized fluids from at least one of the converged drainage paths in the hydrocarbon layer.

  8. Testing Disk Instability Models for Giant Planet Formation

    E-Print Network [OSTI]

    Alan P. Boss

    2007-04-09

    Disk instability is an attractive yet controversial means for the rapid formation of giant planets in our solar system and elsewhere. Recent concerns regarding the first adiabatic exponent of molecular hydrogen gas are addressed and shown not to lead to spurious clump formation in the author's disk instability models. A number of disk instability models have been calculated in order to further test the robustness of the mechanism, exploring the effects of changing the pressure equation of state, the vertical temperature profile, and other parameters affecting the temperature distribution. Possible reasons for differences in results obtained by other workers are discussed. Disk instability remains as a plausible formation mechanism for giant planets.

  9. Benzene formation in the inner regions of protostellar disks

    E-Print Network [OSTI]

    Paul M. Woods; Karen Willacy

    2006-12-08

    Benzene (c-C6H6) formation in the inner 3 AU of a protostellar disk can be efficient, resulting in high abundances of benzene in the midplane region. The formation mechanism is different to that found in interstellar clouds and in protoplanetary nebulae, and proceeds mainly through the reaction between allene (C3H4) and its ion. This has implications for PAH formation, in that some fraction of PAHs seen in the solar system could be native rather than inherited from the interstellar medium.

  10. The Onset of Planet Formation in Brown Dwarf Disks

    E-Print Network [OSTI]

    D. Apai; I. Pascucci; J. Bouwman; A. Natta; Th. Henning; C. P. Dullemond

    2005-11-14

    The onset of planet formation in protoplanetary disks is marked by the growth and crystallization of sub-micron-sized dust grains accompanied by dust settling toward the disk mid-plane. Here we present infrared spectra of disks around brown dwarfs and brown dwarf candidates. We show that all three processes occur in such cool disks in a way similar or identical to that in disks around low- and intermediate-mass stars. These results indicate that the onset of planet formation extends to disks around brown dwarfs, suggesting that planet formation is a robust process occurring in most young circumstellar disks.

  11. Dilute Surfactant Methods for Carbonate Formations

    SciTech Connect (OSTI)

    Kishore K. Mohanty

    2006-02-01

    There are many fractured carbonate reservoirs in US (and the world) with light oil. Waterflooding is effective in fractured reservoirs, if the formation is water-wet. Many fractured carbonate reservoirs, however, are mixed-wet and recoveries with conventional methods are low (less than 10%). The process of using dilute anionic surfactants in alkaline solutions has been investigated in this work for oil recovery from fractured oil-wet carbonate reservoirs both experimentally and numerically. This process is a surfactant-aided gravity drainage where surfactant diffuses into the matrix, lowers IFT and contact angle, which decrease capillary pressure and increase oil relative permeability enabling gravity to drain the oil up. Anionic surfactants have been identified which at dilute concentration of 0.05 wt% and optimal salinity can lower the interfacial tension and change the wettability of the calcite surface to intermediate/water-wet condition as well or better than the cationic surfactant DTAB with a West Texas crude oil. The force of adhesion in AFM of oil-wet regions changes after anionic surfactant treatment to values similar to those of water-wet regions. The AFM topography images showed that the oil-wetting material was removed from the surface by the anionic surfactant treatment. Adsorption studies indicate that the extent of adsorption for anionic surfactants on calcite minerals decreases with increase in pH and with decrease in salinity. Surfactant adsorption can be minimized in the presence of Na{sub 2}CO{sub 3}. Laboratory-scale surfactant brine imbibition experiments give high oil recovery (20-42% OOIP in 50 days; up to 60% in 200 days) for initially oil-wet cores through wettability alteration and IFT reduction. Small (<10%) initial gas saturation does not affect significantly the rate of oil recovery in the imbibition process, but larger gas saturation decreases the oil recovery rate. As the core permeability decreases, the rate of oil recovery reduces, and this reduction can be scaled by the gravitational dimensionless time. Mechanistic simulation of core-scale surfactant brine imbibition matches the experimentally observed imbibition data. In-situ distributions observed through simulation indicate that surfactant diffusion (which depends on temperature and molecular weight) is the rate limiting step. Most of the oil is recovered through gravitational forces. Oil left behind at the end of this process is at its residual oil saturation. The capillary and Bond numbers are not large enough to affect the residual oil saturation. At the field-scale, 50% of the recoverable oil is produced in about 3 years if the fracture spacing is 1 m and 25% if 10 m, in the example simulated. Decreasing fracture spacing and height, increasing permeability, and increasing the extent of wettability alteration increase the rate of oil recovery from surfactant-aided gravity drainage. This dilute surfactant aided gravity-drainage process is relatively cheap. The chemical cost for a barrel of oil produced is expected to be less than $1.

  12. The Recent Cluster Formation Histories of NGC 5253 and NGC 3077: Environmental Impact on Star Formation

    E-Print Network [OSTI]

    J. Harris; D. Calzetti; J. S. Gallagher III; D. A. Smith; C. J. Conselice

    2003-11-20

    We present multicolor photometry of bright star cluster candidates in the nearby starburst galaxies NGC 3077 and NGC 5253, observed with the Hubble Space Telescope Wide Field and Planetary Camera 2 in both broadband (F300W, F547M and F814W) and narrowband (F487N and F656N) filters. By comparing the photometry with theoretical population synthesis models, we estimate the age and mass of each star cluster, which provides constraints on the recent star formation histories of the host galaxies. We compare the star cluster populations in these dwarf starburst galaxies to those of the nuclear starburst in the barred spiral M 83, and discuss implications for our understanding of the nature and evolution of starburst events.

  13. Non-intrusive characterization of heat transfer fluid aerosol formation 

    E-Print Network [OSTI]

    Krishna, Kiran

    2001-01-01

    in process equipment. Predictive models relating the aerosol formation distances, aerosol droplet size, and volume concentrations to bulk liquid pressure, temperature, fluid properties, leak size and ambient conditions are developed. These models will be used...

  14. Nervous Rac: DOCK7 Regulation of Axon Formation

    E-Print Network [OSTI]

    Pinheiro, Elaine Maria

    Microtubules play an important role in neuronal polarity. In this issue of Neuron, Watabe-Uchida et al. link a novel Rac-mediated pathway that regulates microtubule dynamics to axon formation.

  15. DOE Manual Studies 11 Major CO2 Geologic Storage Formations

    Broader source: Energy.gov [DOE]

    A comprehensive study of 11 geologic formations suitable for permanent underground carbon dioxide (CO2) storage is contained in a new manual issued by the U.S. Department of Energy.

  16. Eddy formation and propagation in the eastern tropical Pacific 

    E-Print Network [OSTI]

    Jhingran, Vikas Gopal

    1997-01-01

    Observations of eddies in the eastern tropical Pacific from TOPEX altimetry data show that there are seasonal and interannual variations in eddy activity. Comparisons between time of eddy formation and corresponding wind ...

  17. Looking at Transistor Gate Oxide Formation in Real Time

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Looking at Transistor Gate Oxide Formation in Real Time Print The oxide gate layer is critical to every transistor, and present-day layer thicknesses are in the 10-20 range (1-2...

  18. Energetics of [alpha]-helix formation in peptides and proteins

    E-Print Network [OSTI]

    Schubert, Christian Reinhold

    2009-01-01

    This thesis focuses on the energetics of !-helix formation in peptides and proteins. The [alpha]-helix is the most prevalent type of secondary structure found in proteins, and has arguably dominated our thinking about ...

  19. Star formation histories in early-type galaxies

    E-Print Network [OSTI]

    D. Thomas

    1998-08-24

    I discuss the formation of alpha-enhanced metal-rich stellar populations in the nuclei of luminous ellipticals. Based on hierarchical clustering, different galaxy formation scenarios, which imply different star formation histories, are considered. In contrast to the fast clumpy collapse mode, the late merger of two spiral galaxies fails to reproduce significantly $\\alpha$-enhanced abundance ratios, unless the IMF is flattened. Following the star formation history predicted by semi-analytic models of hierarchical clustering for the average elliptical, solar abundance ratios are obtained with Salpeter IMF. According to the models, bright ellipticals in the field are expected to have significantly lower Mg/Fe ratios than their counterparts in a cluster.

  20. Formation of a compact toroid for enhanced efficiency

    SciTech Connect (OSTI)

    Mozgovoy, A. G. [P.N. Lebedev Physical Institute, Moscow 119991 (Russian Federation)] [P.N. Lebedev Physical Institute, Moscow 119991 (Russian Federation); Romadanov, I. V.; Ryzhkov, S. V., E-mail: ryzhkov@power.bmstu.ru [Bauman Moscow State Technical University, Moscow 105005 (Russian Federation)

    2014-02-15

    We report here our results on the formation of a plasma configuration with the generic name of compact toroid (CT). A method of compact toroid formation to confine, heat and compress a plasma is investigated. Formation of a compact torus using an additional toroidal magnetic field helps to increase the plasma current to a maintainable level of the original magnetic field. We design the Compact Toroid Challenge (CTC) experiment in order to improve the magnetic flux trapping during field reversal in the formation of a compact toroid. The level of the magnetic field immersed in the plasma about 70% of the primary field is achieved. The CTC device and scheme of high level capturing of magnetic flux are presented.

  1. Generating pictures from waves : aspects of image formation

    E-Print Network [OSTI]

    Accardi, Anthony J. (Anthony Joseph), 1976-

    2010-01-01

    The research communities, technologies, and tools for image formation are diverse. On the one hand, computer vision and graphics researchers analyze incoherent light using coarse geometric approximations from optics. On ...

  2. Collisionless Weibel shocks: Full formation mechanism and timing

    SciTech Connect (OSTI)

    Bret, A. [ETSI Industriales, Universidad de Castilla-La Mancha, 13071 Ciudad Real (Spain); Instituto de Investigaciones Energéticas y Aplicaciones Industriales, Campus Universitario de Ciudad Real, 13071 Ciudad Real (Spain); Stockem, A. [GoLP/Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, Lisbon (Portugal); Institut für Theoretische Physik, Lehrstuhl IV: Weltraum- und Astrophysik, Ruhr-Universität Bochum, D-44780 Bochum (Germany); Narayan, R. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-51 Cambridge, Massachusetts 02138 (United States); Silva, L. O. [GoLP/Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, Lisbon (Portugal)

    2014-07-15

    Collisionless shocks in plasmas play an important role in space physics (Earth's bow shock) and astrophysics (supernova remnants, relativistic jets, gamma-ray bursts, high energy cosmic rays). While the formation of a fluid shock through the steepening of a large amplitude sound wave has been understood for long, there is currently no detailed picture of the mechanism responsible for the formation of a collisionless shock. We unravel the physical mechanism at work and show that an electromagnetic Weibel shock always forms when two relativistic collisionless, initially unmagnetized, plasma shells encounter. The predicted shock formation time is in good agreement with 2D and 3D particle-in-cell simulations of counterstreaming pair plasmas. By predicting the shock formation time, experimental setups aiming at producing such shocks can be optimised to favourable conditions.

  3. Environment and the cosmic evolution of star formation

    E-Print Network [OSTI]

    Ravi K. Sheth; Raul Jimenez; Ben Panter; Alan Heavens

    2006-04-27

    We present a mark correlation analysis of the galaxies in the Sloan Digital Sky Survey using weights provided by MOPED. The large size of the sample permits statistically significant statements about how galaxies with different metallicities and star formation histories are spatially correlated. Massive objects formed a larger fraction of their stars at higher redshifts and over shorter timescales than did less massive objects (sometimes called down-sizing). We find that those galaxies which dominated the cosmic star formation at z~3 are predominantly in clusters today, whereas galaxies which dominate the star formation at z~0 inhabit substantially lower mass objects in less dense regions today. Hence, our results indicate that star formation and chemical enrichment occured first in the denser regions of the Universe, and moved to less dense regions at later times.

  4. Determining Multilayer Formation Properties from Transient Temperature and Pressure Measurements 

    E-Print Network [OSTI]

    Sui, Weibo

    2010-10-12

    The Multilayer Transient Test is a well-testing technique designed to determine formation properties in multiple layers, and it has been proved effective during the past two decades. To apply the Multilayer Transient Test, a combination of rate...

  5. Estimating A Shear Modulus Of A Transversely Isotropic Formation

    E-Print Network [OSTI]

    Ellefsen, K. J.

    1990-01-01

    A method to estimate c[subscript 66], which is a shear modulus of a transversely isotropic formation (with its symmetry axis parallel to the borehole), is developed and tested. The inversion for c[subscript 66] is based ...

  6. FORMATION OF COLLOIDAL CRYSTALS FROM NANOPARTICLE STABILIZED COLLOIDAL SUSPENSIONS

    E-Print Network [OSTI]

    Braun, Paul

    FORMATION OF COLLOIDAL CRYSTALS FROM NANOPARTICLE STABILIZED COLLOIDAL SUSPENSIONS BY WENDY WOONYEE.....................................................................8 2.2 Colloid Stability in Suspension .......................................................................................9 2.3 Nanoparticle-Stabilized Colloidal Suspensions...............................................13

  7. Formation and Stability of Impurity “Snakes” in Tokamak Plasmas

    E-Print Network [OSTI]

    Delgado-Aparicio, Luis

    New observations of the formation and dynamics of long-lived impurity-induced helical “snake” modes in tokamak plasmas have recently been carried out on Alcator C-Mod. The snakes form as an asymmetry in the impurity ion ...

  8. Rapid gas hydrate formation processes: Will they work?

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Brown, Thomas D.; Taylor, Charles E.; Bernardo, Mark P.

    2010-06-07

    Researchers at DOE’s National Energy Technology Laboratory (NETL) have been investigating the formation of synthetic gas hydrates, with an emphasis on rapid and continuous hydrate formation techniques. The investigations focused on unconventional methods to reduce dissolution, induction, nucleation and crystallization times associated with natural and synthetic hydrates studies conducted in the laboratory. Numerous experiments were conducted with various high-pressure cells equipped with instrumentation to study rapid and continuous hydrate formation. The cells ranged in size from 100 mL for screening studies to proof-of-concept studies with NETL’s 15-Liter Hydrate Cell. The results from this work demonstrate that the rapid and continuousmore »formation of methane hydrate is possible at predetermined temperatures and pressures within the stability zone of a Methane Hydrate Stability Curve.« less

  9. Acid Fracturing Feasibility Study for Heterogeneous Carbonate Formation 

    E-Print Network [OSTI]

    Suleimenova, Assiya

    2015-03-03

    Acid fracturing is a stimulation technique that is commonly used by the industry to increase productivity or injectivity of wells in carbonate reservoirs. To determine a feasibility of acid fracturing treatment for a heterogeneous formation...

  10. A PKN Hydraulic Fracture Model Study and Formation Permeability Determination 

    E-Print Network [OSTI]

    Xiang, Jing

    2012-02-14

    Hydraulic fracturing is an important method used to enhance the recovery of oil and gas from reservoirs, especially for low permeability formations. The distribution of pressure in fractures and fracture geometry are needed to design conventional...

  11. Formation Damage due to CO2 Sequestration in Saline Aquifers 

    E-Print Network [OSTI]

    Mohamed, Ibrahim Mohamed 1984-

    2012-10-25

    Carbon dioxide (CO2) sequestration is defined as the removal of gas that would be emitted into the atmosphere and its subsequent storage in a safe, sound place. CO2 sequestration in underground formations is currently being considered to reduce...

  12. Network Formation in the Presence of Contagious Risk Larry Blume

    E-Print Network [OSTI]

    Kleinberg, Robert D.

    Network Formation in the Presence of Contagious Risk Larry Blume David Easley Jon Kleinberg-linking" in networks with contagious risk can have strong consequences for the welfare of the participants. 1

  13. Quasi Light Fields: A Model of Coherent Image Formation

    E-Print Network [OSTI]

    Accardi, Anthony J.

    We develop a model of coherent image formation that strikes a balance between the simplicity of the light field and the comprehensive predictive power of Maxwell's equations, by extending the light field to coherent radiation.

  14. Optimal Multi-Temperature delivery frequency for small format stores

    E-Print Network [OSTI]

    Barooah, Mayurpankhi

    2015-01-01

    Retailers are exploring more efficient ways to deliver to small format stores that demand frequent and small volume deliveries from Distribution Centers. The need to deliver products at different temperatures, viz. Ambient, ...

  15. Nonequilibrium pattern formation in strongly interacting driven colloids

    E-Print Network [OSTI]

    Dzubiella, Joachim

    formation are relevant on the route into the stratified steady state. I. Introduction Almost fifty years ago in highly charged and strongly deionized sus- pensions which exhibit strong correlations even at very low

  16. Post-Formative Ceramics in the Eastern Grat Basin

    E-Print Network [OSTI]

    Forsyth, Donald W

    1986-01-01

    Great Salt Lake Fremont Ceramics. In: The Levee Site and the1986). Post-Formative Ceramics in the Eastern Great Basin: A1977 Prehistoric Ceramics of the Fremont. Museiun of

  17. Suppression of Cavity Formation in Ceramics: Prospects for Superplasticity

    E-Print Network [OSTI]

    Suppression of Cavity Formation in Ceramics: Prospects for Superplasticity A. G. EVANS* Materials, Ohio State University, Columbus, Ohio 43210 Ceramics exhibit macroscopic stressistrain rate relations- tive surface diffusivities must be selected. I. Introduction HEN polycrystalline ceramic materials

  18. Polymorphism control and the formation of organic molecular nanocrystals

    E-Print Network [OSTI]

    Yang, Xiaochuan, Ph. D. Massachusetts Institute of Technology

    2014-01-01

    The formation of organic molecular nanocrystals is a topic of great interest in the pharmaceutical industry because of the potential increase in dissolution rate and solubility of organic crystals below 1 ptm and their ...

  19. Formation lengths of hadrons in lepto-production

    E-Print Network [OSTI]

    Levon Grigoryan

    2012-09-28

    The average formation lengths of the hadrons produced during the deep inelastic scattering (DIS) of leptons on protons are studied in the framework of the symmetric Lund model. It is shown that these formation lengths essentially depend on the electric charges of the hadron. For electro-production and charged current (CC) neutrino-production, the average formation lengths of positively charged particles are larger than those of negatively charged antiparticles. This situation is reversed for CC antineutrino-production. In all the mentioned cases, the main mechanism is the direct production of hadrons. The additional mechanism of hadron production, through the decay of resonances, is essential only for pions and leads to a decrease in the average formation lengths.

  20. Clarifying the Dominant Sources and Mechanisms of Cirrus Cloud Formation

    E-Print Network [OSTI]

    Cziczo, Daniel James

    Formation of cirrus clouds depends on the availability of ice nuclei to begin condensation of atmospheric water vapor. Although it is known that only a small fraction of atmospheric aerosols are efficient ice nuclei, the ...

  1. The Complexity of Rationalizing Network Formation Shankar Kalyanaraman

    E-Print Network [OSTI]

    Umans, Chris

    and the Inequality-SAT (I-SAT) problem. Finally and most significantly, we prove that an approximation version. Keywords-network formation games, rationalization, Jackson- Wolinsky model, Inequality-SAT, hardness

  2. Rapid Gas Hydrate Formation Processes: Will They Work?

    SciTech Connect (OSTI)

    Brown, Thomas D.; Taylor, Charles E.; Bernardo, Mark P.

    2010-06-01

    Researchers at DOE’s National Energy Technology Laboratory (NETL) have been investigating the formation of synthetic gas hydrates, with an emphasis on rapid and continuous hydrate formation techniques. The investigations focused on unconventional methods to reduce dissolution, induction, nucleation and crystallization times associated with natural and synthetic hydrates studies conducted in the laboratory. Numerous experiments were conducted with various high-pressure cells equipped with instrumentation to study rapid and continuous hydrate formation. The cells ranged in size from 100 mL for screening studies to proof-of-concept studies with NETL’s 15-Liter Hydrate Cell. Results from this work demonstrate that the rapid and continuous formation of methane hydrate is possible at predetermined temperatures and pressures within the stability zone of a Methane Hydrate Stability Curve.

  3. Star Formation in Mergers and Interacting Galaxies: Gathering the Fuel

    E-Print Network [OSTI]

    Curtis Struck

    2006-10-06

    Selected results from recent studies of star formation in galaxies at different stages of interaction are reviewed. Recent results from the Spitzer Space Telescope are highlighted. Ideas on how large-scale driving of star formation in interacting galaxies might mesh with our understanding of star formation in isolated galaxies and small scale mechanisms within galaxies are considered. In particular, there is evidence that on small scales star formation is determined by the same thermal and turbulent processes in cool compressed clouds as in isolated galaxies. If so, this affirms the notion that the primary role of large-scale dynamics is to gather and compress the gas fuel. In gas-rich interactions this is generally done with increasing efficiency through the merger process.

  4. Formation of molecules in an expanding Bose-Einstein condensate

    E-Print Network [OSTI]

    V. A. Yurovsky; A. Ben-Reuven

    2004-02-12

    A mean field theory of expanding hybrid atom-molecule Bose-Einstein condensates is applied to the recent MPI experiments on ${}^{87}$Rb that demonstrated the formation of ultracold molecules due to Feshbach resonance. The subsequent dissociation of the molecules is treated using a non-mean-field parametric approximation. The latter method is also used in determining optimal conditions for the formation of molecular BEC

  5. Formation, regeneration and fusion of protoplasts from Gliocladium spp. 

    E-Print Network [OSTI]

    Seh, Monica Leigh

    1987-01-01

    FORMATION, REGENERATION AND FUSION OF PROTOPLASTS FROM GLIOCLADIUM SPP. A Thesis by MONICA LEIGH SEH Submitted to the Graduate College of Texas ARM University in partial fulfillment of the requirements of the degree of MASTER OF SCIENCE... August 1987 Major Subject: Plant Pathology FORMATION, REGENERATION AND FUSION OF PROTOPLASTS FROM GLIOCLADIUM SPP. A Thesis MONICA LEIGH SEH Approved as to style and content by: Charles M. X nerle (Chairperson of Committee) ic ael D. Thomas...

  6. Recipes for ULX formation: necessary ingredients and garnishments

    E-Print Network [OSTI]

    Roberto Soria

    2006-11-05

    I summarize the main observational features that seem to recur more frequently in the ULX population. I speculate that two of the most important physical requirements for ULX formation are low metal abundance, and clustered star formation triggered by external processes such as molecular cloud collisions. In this scenario, most ULX are formed from recent stellar processes, have BH masses < 100 Msun and do not require merger processes in super star clusters.

  7. Dynamics of precipitation pattern formation at geothermal hot springs

    E-Print Network [OSTI]

    Nigel Goldenfeld; Pak Yuen Chan; John Veysey

    2006-05-26

    We formulate and model the dynamics of spatial patterns arising during the precipitation of calcium carbonate from a supersaturated shallow water flow. The model describes the formation of travertine deposits at geothermal hot springs and rimstone dams of calcite in caves. We find explicit solutions for travertine domes at low flow rates, identify the linear instabilities which generate dam and pond formation on sloped substrates, and present simulations of statistical landscape evolution.

  8. The star formation main sequence and stellar mass assembly of galaxies in the Illustris simulation

    E-Print Network [OSTI]

    Sparre, Martin

    Understanding the physical processes that drive star formation is a key challenge for galaxy formation models. In this paper, we study the tight correlation between the star formation rate (SFR) and stellar mass of galaxies ...

  9. The Mechanism of First Raindrops Formation in Deep Convective Clouds

    SciTech Connect (OSTI)

    Khain, Alexander; Prabha, Thara; Benmoshe, Nir; Pandithurai, G.; Ovchinnikov, Mikhail

    2013-08-22

    The formation of first raindrops in deep convective clouds is investigated. A combination of observational data analysis and 2-D and 3-D numerical bin microphysical simulations of deep convective clouds suggests that the first raindrops form at the top of undiluted or slightly diluted cores. It is shown that droplet size distributions in these regions are wider and contain more large droplets than in diluted volumes. The results of the study indicate that the initial raindrop formation is determined by the basic microphysical processes within ascending adiabatic volumes. It allows one to predict the height of the formation of first raindrops considering the processes of nucleation, diffusion growth and collisions. The results obtained in the study explain observational results reported by Freud and Rosenfeld (2012) according to which the height of first raindrop formation depends linearly on the droplet number concentration at cloud base. The results also explain why a simple adiabatic parcel model can reproduce this dependence. The present study provides a physical basis for retrieval algorithms of cloud microphysical properties and aerosol properties using satellites proposed by Rosenfeld et al. ( 2012). The study indicates that the role of mixing and entrainment in the formation of the first raindrops is not of crucial importance. It is also shown that low variability of effective and mean volume radii along horizontal traverses, as regularly observed by in situ measurements, can be simulated by high-resolution cloud models, in which mixing is parameterized by a traditional 1.5 order turbulence closure scheme.

  10. Clustering and pattern formation in chemorepulsive active colloids

    E-Print Network [OSTI]

    Benno Liebchen; Davide Marenduzzo; Ignacio Pagonabarraga; Michael E. Cates

    2015-08-19

    We present a model for the collective dynamics of a suspension of active colloidal particles, whose motion is driven by gradients in the concentration of a chemical that they produce. For the chemorepulsive case, where particles migrate away from their chemical product, we predict two new generic mechanisms causing microphase separation and pattern formation. The first such mechanism leads to the formation of stable clusters of a finite size, and relies on an anisotropy in chemical production at the particle surface, as expected for synthetic active colloids (Janus spheres) that move by autophoresis. These clusters, whose size increases with activity, are each stabilized by a chemorepellent shell that keeps the particles in the cluster together while driving other clusters away. Our second route to pattern formation arises even in the absence of such anisotropy, through oscillations caused by a delay in the reorientation response of the active colloids to local gradients in the chemical density field. This leads to formation of dynamical clusters that often, but not always, settle into a travelling wave pattern. Finally we find that a competition of these two mechanism can create a pattern of "blinking clusters" that continuously exchange particles with each other. These new mechanisms for the formation of dynamic, finite-sized clusters in active matter might help explain recent experimental findings. More generally, they point to novel design principles for self-assembly of active colloids into spatiotemporal patterns.

  11. nIFTy Cosmology: Comparison of Galaxy Formation Models

    E-Print Network [OSTI]

    Knebe, Alexander; Thomas, Peter A; Benson, Andrew; Blaizot, Jeremy; Bower, Richard; Carretero, Jorge; Castander, Francisco J; Cattaneo, Andrea; Cora, Sofia A; Croton, Darren J; Cui, Weiguang; Cunnama, Daniel; De Lucia, Gabriella; Devriendt, Julien E; Elahi, Pascal J; Font, Andreea; Fontanot, Fabio; Garcia-Bellido, Juan; Gargiulo, Ignacio D; Gonzalez-Perez, Violeta; Helly, John; Henriques, Bruno; Hirschmann, Michaela; Lee, Jaehyun; Mamon, Gary A; Monaco, Pierluigi; Onions, Julian; Padilla, Nelson D; Power, Chris; Pujol, Arnau; Skibba, Ramin A; Somerville, Rachel S; Srisawat, Chaichalit; Vega-Martinez, Cristian A; Yi, Sukyoung K

    2015-01-01

    We present a comparison of 14 galaxy formation models: 12 different semi-analytical models and 2 halo-occupation distribution models for galaxy formation based upon the same cosmological simulation and merger tree information derived from it. The participating codes have proven to be very successful in their own right but they have all been calibrated independently using various observational data sets, stellar models, and merger trees. In this paper we apply them without recalibration and this leads to a wide variety of predictions for the stellar mass function, specific star formation rates, stellar-to- halo mass ratios, and the abundance of orphan galaxies. The scatter is much larger than seen in previous comparison studies primarily because the codes have been used outside of their native environment within which they are well tested and calibrated. The purpose of the `nIFTy comparison of galaxy formation models' is to bring together as many different galaxy formation modellers as possible and to investig...

  12. On The History and Future of Cosmic Planet Formation

    E-Print Network [OSTI]

    Behroozi, Peter

    2015-01-01

    We combine constraints on galaxy formation histories with planet formation models, yielding the Earth-like and giant planet formation histories of the Milky Way and the Universe as a whole. In the Hubble Volume (10^13 Mpc^3), we expect there to be ~10^20 Earth-like and ~10^20 giant planets; our own galaxy is expected to host ~10^9 and ~10^10 Earth-like and giant planets, respectively. Proposed metallicity thresholds for planet formation do not significantly affect these numbers. However, the metallicity dependence for giant planets results in later typical formation times and larger host galaxies than for Earth-like planets. The Solar System formed at the median age for existing giant planets in the Milky Way, and consistent with past estimates, formed after 80% of Earth-like planets. However, if existing gas within virialised dark matter haloes continues to collapse and form stars and planets, the Universe will form over 10 times more planets than currently exist. We show that this would imply at least a 92%...

  13. Heating hydrocarbon containing formations in a line drive staged process

    DOE Patents [OSTI]

    Miller, David Scott (Katy, TX)

    2009-07-21

    Method for treating a hydrocarbon containing formation are described herein. Methods may include providing heat to a first section of the formation with one or more first heaters in the first section. First hydrocarbons may be heated in the first section such that at least some of the first hydrocarbons are mobilized. At least some of the mobilized first hydrocarbons may be produced through a production well located in a second section of the formation. The second section may be located substantially adjacent to the first section. A portion of the second section may be provided some heat from the mobilized first hydrocarbons, but is not conductively heated by heat from the first heaters. Heat may be provided to the second section with one or more second heaters in the second section to further heat the second section.

  14. HD 80606: Searching the chemical signature of planet formation

    E-Print Network [OSTI]

    Saffe, C; Buccino, A

    2015-01-01

    (Abridged) Binary systems with similar components are ideal laboratories which allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process. Aims. We explore the probable chemical signature of planet formation in the remarkable binary system HD 80606 - HD 80607. The star HD 80606 hosts a giant planet with 4 MJup detected by both transit and radial velocity techniques, being one of the most eccentric planets detected to date. We study condensation temperature Tc trends of volatile and refractory element abundances to determine whether there is a depletion of refractories that could be related to the terrestrial planet formation. Methods. We carried out a high-precision abundance determination in both components of the binary system, using a line-by-line strictly differential approach, using the Sun as a reference and then using HD 80606 as reference. We used an updated version of the program FUNDPAR, together with ATLAS9 model atmospheres and th...

  15. Solar System Formation Deduced from Observations of Matter

    E-Print Network [OSTI]

    Herndon, J M

    2004-01-01

    Aspects of our Solar System's formation are deduced from observations of the chemical nature of matter. Massive cores are indicative of terrestrial-planet-composition-similarity to enstatite chondrite meteorites, whose highly-reduced state of oxidation may be thermodynamically stable in solar matter only at elevated temperatures and pressures. Consistent with the formation of Earth as envisioned by Arnold Eucken, thermodynamic considerations lead to the deduction that the terrestrial planets formed by liquid-condensation, raining out from the central regions of hot, gaseous protoplanets. The mass of protoplanetary-Earth, estimated to be 275-305mE, is similar to the mass of Jupiter, 318mE. Solar primordial gases and volatile elements were separated from the terrestrial planets early after planet formation, presumably during some super-luminous solar event, perhaps even before Mercury had completely formed. The pre-super-luminosity-terrestrial-planet mass distribution appears to be more consistent with observat...

  16. Kinetics of bond formation in crosslinked gelatin gels

    E-Print Network [OSTI]

    T. Abete; E. Del Gado; D. Hellio Serughetti; L. de Arcangelis; M. Djabourov; A. Coniglio

    2006-11-07

    In chemical crosslinking of gelatin solutions, two different time scales affect the kinetics of the gel formation in the experiments. We complement the experimental study with Monte Carlo numerical simulations of a lattice model. This approach shows that the two characteristic time scales are related to the formation of single bonds crosslinker-chain and of bridges between chains. In particular their ratio turns out to control the kinetics of the gel formation. We discuss the effect of the concentration of chains. Finally our results suggest that, by varying the probability of forming bridges as an independent parameter, one can finely tune the kinetics of the gelation via the ratio of the two characteristic times.

  17. Bump formation in a binary attractor neural network

    SciTech Connect (OSTI)

    Koroutchev, Kostadin; Korutcheva, Elka

    2006-02-15

    The conditions for the formation of local bumps in the activity of binary attractor neural networks with spatially dependent connectivity are investigated. We show that these formations are observed when asymmetry between the activity during the retrieval and learning is imposed. An analytical approximation for the order parameters is derived. The corresponding phase diagram shows a relatively large and stable region where this effect is observed, although critical storage and information capacities drastically decrease inside that region. We demonstrate that the stability of the network, when starting from the bump formation, is larger than the stability when starting even from the whole pattern. Finally, we show a very good agreement between the analytical results and the simulations performed for different topologies of the network.

  18. Galaxy formation history through hod model from euclid mock catalogs

    E-Print Network [OSTI]

    Sakr, Ziad

    2015-01-01

    Halo Occupation Distribution (HOD) is a model giving the average number of galaxies in a dark matter halo, function of its mass and other intrinsic properties, like distance from halo center, luminosity and redshift of its constituting galaxies. It is believed that these parameters could also be related to the galaxy history of formation. We want to investigate more this relation in order to test and better refine this model. To do that, we extract HOD indicators from EUCLID mock catalogs for different luminosity cuts and for redshifts ranges going from 0.1 formation history following the idea that galaxy evolution is the combination rather than the conflict of the two main proposed ideas nowadays: the older hierarchical mass merger driven paradigm and the recent downsizing star formation driven approach.

  19. Effects of the UV background radiation on galaxy formation

    E-Print Network [OSTI]

    Masahiro Nagashima; Naoteru Gouda; Norimasa Sugiura

    1999-06-10

    We investigate the effects of the UV background radiation on galaxy formation by using the semi-analytic model including the photoionization process. The semi-analytic model is based on Cole et al. (1994) and we use almost the same parameters of their `fiducial' model. We find that the UV background mainly affects the formation of dwarf galaxies. Because of the suppression of star formation, the number density of small objects corresponding to dwarf galaxies decreases compared to the case of no UV radiation when the UV background exists until the present epoch. When the UV background vanishes at a low redshift, the number density of small objects is hardly changed but the colour becomes bluer, compared to the case of no UV radiation, because stars are newly formed after the UV background vanishes. On the other hand, the UV radiation hardly affects massive galaxies. This is because the massive galaxies are formed by mergers of small galaxies.

  20. Microchannel formation in seaice as habitat for microalgae

    E-Print Network [OSTI]

    K. Morawetz; S. Thoms; B. Kutschan

    2014-07-08

    The formation of saline brine channels in seaice is described by two coupled order parameters, the tetrahedricity as structure of ice and the salinity. Their evolution equations follow from a Ginzburg-Landau-functional in the form of a phase-field theory conserving salinity. The stability analysis provides the phase diagram in terms of two parameters, one describing the velocity of the freezing process and the other one characterizing the velocity of structure formation. In thermodynamics these parameters determine the supercooling or superheating region and the specific heat respectively. In contrast to the Turing model the diffusivity does not enter this phase diagram but determines only the structure size. The numerical solution shows a microstructure formation of brine inclusions in agreement with the measured samples dependent on the salinity and temperature.

  1. Heating hydrocarbon containing formations in a spiral startup staged sequence

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Miller, David Scott (Katy, TX)

    2009-12-15

    Methods for treating a hydrocarbon containing formation are described herein. Methods may include treating a first zone of the formation. Treatment of a plurality of zones of the formation may be begun at selected times after the treatment of the first zone begins. The treatment of at least two successively treated zones may begin at a selected time after treatment of the previous zone begins. At least two of the successively treated zones may be adjacent to the zone treated previously. The successive treatment of the zones proceeds in an outward, substantially spiral sequence from the first zone so that the treatment of the zones may move substantially spirally outwards towards a boundary of the treatment area.

  2. Solar System Processes Underlying Planetary Formation, Geodynamics, and the Georeactor

    E-Print Network [OSTI]

    Herndon, J M

    2006-01-01

    Only three processes, operant during the formation of the Solar System, are responsible for the diversity of matter in the Solar System and are directly responsible for planetary internal-structures, including planetocentric nuclear fission reactors, and for dynamical processes, including and especially, geodynamics. These processes are: (i) Low-pressure, low-temperature condensation from solar matter in the remote reaches of the Solar System or in the interstellar medium; (ii) High-pressure, high-temperature condensation from solar matter associated with planetary-formation by raining out from the interiors of giant-gaseous protoplanets, and; (iii) Stripping of the primordial volatile components from the inner portion of the Solar System by super-intense solar wind associated with T-Tauri phase mass-ejections, presumably during the thermonuclear ignition of the Sun. As described herein, these processes lead logically, in a causally related manner, to a coherent vision of planetary formation with profound imp...

  3. The Formation of a Bubble from a Submerged Orifice

    E-Print Network [OSTI]

    Simmons, Jonathan A; Shikhmurzaev, Yulii D

    2015-01-01

    The formation of a single bubble from an orifice in a solid surface, submerged in an in- compressible, viscous Newtonian liquid, is simulated. The finite element method is used to capture the multiscale physics associated with the problem and to track the evolution of the free surface explicitly. The results are compared to a recent experimental analysis and then used to obtain the global characteristics of the process, the formation time and volume of the bubble, for a range of orifice radii; Ohnesorge numbers, which combine the material parameters of the liquid; and volumetric gas flow rates. These benchmark calculations, for the parameter space of interest, are then utilised to validate a selection of scaling laws found in the literature for two regimes of bubble formation, the regimes of low and high gas flow rates.

  4. GAMMA RAYS FROM STAR FORMATION IN CLUSTERS OF GALAXIES

    SciTech Connect (OSTI)

    Storm, Emma M.; Jeltema, Tesla E.; Profumo, Stefano [Department of Physics, University of California, 1156 High Street, Santa Cruz, CA 95064 (United States)

    2012-08-20

    Star formation in galaxies is observed to be associated with gamma-ray emission, presumably from non-thermal processes connected to the acceleration of cosmic-ray nuclei and electrons. The detection of gamma rays from starburst galaxies by the Fermi Large Area Telescope (LAT) has allowed the determination of a functional relationship between star formation rate and gamma-ray luminosity. Since star formation is known to scale with total infrared (8-1000 {mu}m) and radio (1.4 GHz) luminosity, the observed infrared and radio emission from a star-forming galaxy can be used to quantitatively infer the galaxy's gamma-ray luminosity. Similarly, star-forming galaxies within galaxy clusters allow us to derive lower limits on the gamma-ray emission from clusters, which have not yet been conclusively detected in gamma rays. In this study, we apply the functional relationships between gamma-ray luminosity and radio and IR luminosities of galaxies derived by the Fermi Collaboration to a sample of the best candidate galaxy clusters for detection in gamma rays in order to place lower limits on the gamma-ray emission associated with star formation in galaxy clusters. We find that several clusters have predicted gamma-ray emission from star formation that are within an order of magnitude of the upper limits derived in Ackermann et al. based on non-detection by Fermi-LAT. Given the current gamma-ray limits, star formation likely plays a significant role in the gamma-ray emission in some clusters, especially those with cool cores. We predict that both Fermi-LAT over the course of its lifetime and the future Cerenkov Telescope Array will be able to detect gamma-ray emission from star-forming galaxies in clusters.

  5. Method and apparatus for production of subsea hydrocarbon formations

    DOE Patents [OSTI]

    Blandford, Joseph W. (15 Mott La., Houston, TX 77024)

    1995-01-01

    A system for controlling, separating, processing and exporting well fluids produced from subsea hydrocarbon formations is disclosed. The subsea well tender system includes a surface buoy supporting one or more decks above the water surface for accommodating equipment to process oil, gas and water recovered from the subsea hydrocarbon formation. The surface buoy includes a surface-piercing central flotation column connected to one or more external floatation tanks located below the water surface. The surface buoy is secured to the seabed by one or more tendons which are anchored to a foundation with piles imbedded in the seabed. The system accommodates multiple versions on the surface buoy configuration.

  6. Method for maximizing shale oil recovery from an underground formation

    DOE Patents [OSTI]

    Sisemore, Clyde J. (Livermore, CA)

    1980-01-01

    A method for maximizing shale oil recovery from an underground oil shale formation which has previously been processed by in situ retorting such that there is provided in the formation a column of substantially intact oil shale intervening between adjacent spent retorts, which method includes the steps of back filling the spent retorts with an aqueous slurry of spent shale. The slurry is permitted to harden into a cement-like substance which stabilizes the spent retorts. Shale oil is then recovered from the intervening column of intact oil shale by retorting the column in situ, the stabilized spent retorts providing support for the newly developed retorts.

  7. Vesicle dynamics in elongation flow: Wrinkling instability and bud formation

    E-Print Network [OSTI]

    Vasiliy Kantsler; Enrico Segre; Victor Steinberg

    2007-04-30

    We present experimental results on the relaxation dynamics of vesicles subjected to a time-dependent elongation flow. We observed and characterized a new instability, which results in the formation of higher order modes of the vesicle shape (wrinkles), after a switch in the direction of the gradient of the velocity. This surprising generation of membrane wrinkles can be explained by the appearance of a negative surface tension during the vesicle deflation, due to compression in a sign-switching transient. Moreover, the formation of buds in the vesicle membrane has been observed in the vicinity of the dynamical transition point.

  8. Vesicle dynamics in elongation flow: Wrinkling instability and bud formation

    E-Print Network [OSTI]

    Kantsler, Vasiliy; Steinberg, Victor; 10.1103/PhysRevLett.99.178102

    2011-01-01

    We present experimental results on the relaxation dynamics of vesicles subjected to a time-dependent elongation flow. We observed and characterized a new instability, which results in the formation of higher order modes of the vesicle shape (wrinkles), after a switch in the direction of the gradient of the velocity. This surprising generation of membrane wrinkles can be explained by the appearance of a negative surface tension during the vesicle deflation, due to compression in a sign-switching transient. Moreover, the formation of buds in the vesicle membrane has been observed in the vicinity of the dynamical transition point.

  9. Formation of carbon deposits from coal in an arc plasma

    SciTech Connect (OSTI)

    Wang, B.; Tian, Y.; Zhang, Y.; Zhu, S.; Lu, Y.; Zhang, Y.; Xie, K.

    2007-07-01

    The issue of deposited carbon (DC) on a reactor wall during the production of acetylene by the coal/arc plasma process is a potential obstacle for the industrialization process. The formation mechanism of DC is very difficult to reveal because the high complexity of coal and the volatile matter. Combining with quenching technique, the methane, liquid petroleum gas and benzene were employed as the model materials to roughly act as the light gas, chain and aromatic subcomponents of volatile matter, and then the reasonable formation mechanism of DC was subtly speculated accordingly.

  10. Mechanism of membrane tube formation induced by adhesive nanocomponents

    E-Print Network [OSTI]

    Šari?, Andela

    2015-01-01

    We report numerical simulations of membrane tubulation driven by large colloidal particles. Using Monte Carlo simulations we study how the process depends on particle size, concentration and binding strength, and present accurate free energy calculations to sort out how tube formation compares with the competing budding process. We find that tube formation is a result of the collective behavior of the particles adhering on the surface, and it occurs for binding strengths that are smaller than those required for budding. We also find that long linear aggregates of particles forming on the membrane surface act as nucleation seeds for tubulation by lowering the free energy barrier associated to the process.

  11. Method and apparatus for production of subsea hydrocarbon formations

    DOE Patents [OSTI]

    Blandford, J.W.

    1995-01-17

    A system for controlling, separating, processing and exporting well fluids produced from subsea hydrocarbon formations is disclosed. The subsea well tender system includes a surface buoy supporting one or more decks above the water surface for accommodating equipment to process oil, gas and water recovered from the subsea hydrocarbon formation. The surface buoy includes a surface-piercing central flotation column connected to one or more external flotation tanks located below the water surface. The surface buoy is secured to the sea bed by one or more tendons which are anchored to a foundation with piles imbedded in the sea bed. The system accommodates multiple versions on the surface buoy configuration. 20 figures.

  12. Spontaneous Superlattice Formation in Nanorods through PartialCation Exchange

    SciTech Connect (OSTI)

    Robinson, Richard D.; Sadtler, Bryce; Demchenko, Denis O.; Erdonmez, Can K.; Wang, Lin-Wang; Alivisatos, A. Paul

    2007-03-14

    Lattice mismatch strains are widely known to controlnanoscale pattern formation in heteroepitaxy, but such effects have notbeen exploited in colloidal nanocrystal growth. We demonstrate acolloidal route to synthesizing CdS-Ag2S nanorod superlattices throughpartial cation exchange. Strain induces the spontaneous formation ofperiodic structures. Ab initio calculations of the interfacial energy andmodeling of strain energies show that these forces drive theself-organization. The nanorod superlattices exhibit high stabilityagainst ripening and phase mixing. These materials are tunablenear-infrared emitters with potential applications as nanometer-scaleoptoelectronic devices.

  13. TEXAS A&M UNIVERSITY LIBRARIES USING THE CHICAGO MANUAL OF STYLE (CMOS) FORMAT

    E-Print Network [OSTI]

    Liberia, 1833-1869. Lexington: University Press of Kentucky. #12;Using Chicago Manual of Style Format

  14. Basics of Polar-Format algorithm for processing Synthetic Aperture Radar images.

    SciTech Connect (OSTI)

    Doerry, Armin Walter

    2012-05-01

    The purpose of this report is to provide a background to Synthetic Aperture Radar (SAR) image formation using the Polar Format (PFA) processing algorithm. This is meant to be an aid to those tasked to implement real-time image formation using the Polar Format processing algorithm.

  15. Solution mining and heating by oxidation for treating hydrocarbon containing formations

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Stegemeier, George Leo (Houston, TX)

    2009-06-23

    A method for treating an oil shale formation comprising nahcolite includes providing a first fluid to a portion of the formation. A second fluid is produced from the portion. The second fluid includes at least some nahcolite dissolved in the first fluid. A controlled amount of oxidant is provided to the portion of the formation. Hydrocarbon fluids are produced from the formation.

  16. Secondary state formation during the early iron age on the island of Sri Lanka : the evolution of a periphery

    E-Print Network [OSTI]

    Karunaratne, Priyantha Padmalal

    2010-01-01

    Chicago, Illinois, in (52) Symposium- Beyond basic formationIllinois. March 1999. xx ABSTRACT OF THE DISSERTATION Secondary State Formation

  17. Method of condensing vaporized water in situ to treat tar sands formations

    DOE Patents [OSTI]

    Hsu, Chia-Fu (Rijswijk, NL)

    2010-03-16

    Methods for treating a tar sands formation are described herein. Methods may include heating at least a section of a hydrocarbon layer in the formation from a plurality of heaters located in the formation. Heat may be allowed to transfer from the heaters to at least a first portion of the formation. Conditions may be controlled in the formation so that water vaporized by the heaters in the first portion is selectively condensed in a second portion of the formation. At least some of the fluids may be produced from the formation.

  18. Controlled Irradiative Formation of Penitentes Vance Bergeron,1

    E-Print Network [OSTI]

    Betterton, Meredith D.

    , further growth of height can occur by melting. The penitentes initially appear as small structures (3 mm in troughs and surface instability [1­3]. Penitente formation alters glacial energy balances and therefore (dew point below 0 C), where melting is disfavored and abla- tion proceeds by sublimation [4

  19. Overview of Lead Scale Formation and Solubility J. Barry Maynard

    E-Print Network [OSTI]

    Maynard, J. Barry

    Overview of Lead Scale Formation and Solubility J. Barry Maynard University of Cincinnati 2008 The response of lead source materials in premise and distribution systems to changes in water treatment. These determinations are particularly critical for lead compounds, of which there have been many reported. Knowledge

  20. Well completion process for formations with unconsolidated sands

    DOE Patents [OSTI]

    Davies, David K. (Kingwood, TX); Mondragon, III, Julius J. (Redondo Beach, CA); Hara, Philip Scott (Monterey Park, CA)

    2003-04-29

    A method for consolidating sand around a well, involving injecting hot water or steam through well casing perforations in to create a cement-like area around the perforation of sufficient rigidity to prevent sand from flowing into and obstructing the well. The cement area has several wormholes that provide fluid passageways between the well and the formation, while still inhibiting sand inflow.

  1. Tuesday, March 13, 2007 SOLAR SYSTEM FORMATION AND EVOLUTION

    E-Print Network [OSTI]

    Rathbun, Julie A.

    Tuesday, March 13, 2007 SOLAR SYSTEM FORMATION AND EVOLUTION 8:30 a.m. Marina Plaza Ballroom Chairs into Protoplanetary Disks [#1909] We build on our previous simulations of supernova ejecta hitting protoplanetary. M. García-Lario P. Manchado A. Massive AGB Stars in the Early Solar System? [#1879] We present

  2. Network Formation and Routing by Strategic Agents using Local Contracts

    E-Print Network [OSTI]

    Anshelevich, Elliot

    Network Formation and Routing by Strategic Agents using Local Contracts Elliot Anshelevich1, Murray Hill, NJ. Abstract. The Internet consists of various independent entities that range from small their business goals. For example, customers accept contracts with ISPs to connect them to the Internet while

  3. Evaluation of the Azinomycin B Biosynthetic Pathway: The Azabicycle Formation 

    E-Print Network [OSTI]

    Lee, Rachel Pokei

    2014-01-02

    on the overall biosynthesis of azinomycin B. Previous attempt to characterize AziC2 suggested that the first step of azinomycin B’s azabicycle fragment formation involves the transfer of L-glutamate, the amino-acid precursor, to downstream biosynthetic enzymes...

  4. Modelling of reoxidation inclusion formation in steel sand casting

    E-Print Network [OSTI]

    Beckermann, Christoph

    Modelling of reoxidation inclusion formation in steel sand casting A. J. Melendez, K. D. Carlson pouring, as well as their final locations on the surface of steel sand castings. Inclusions originate. The inclusion model is implemented in a general-purpose casting simulation code. The model is validated

  5. Modeling of NOx formation in circular laminar jet flames 

    E-Print Network [OSTI]

    Siwatch, Vivek

    2007-04-25

    of air entrainment by jet depends upon the Sc number of fuel. The higher the Sc number, the higher is the air entrained which lowers the flame temperature and hence NOx formation. With increasing Sc number, flame volume increases which leads...

  6. Modeling of magnetic island formation in magnetic reconnection experiment

    E-Print Network [OSTI]

    Ji, Hantao

    the spontaneous FRC formation with effective plasma heating by magnetic reconnection.6 In the Magnetic, Gifu, 509-5292, Japan M. Yamada and H. Ji Plasma Physics Laboratory, Princeton University, Princeton found in the Magnetic Reconnection Experiment MRX M. Yamada, H. Ji, S. Hsu, et al., Phys. Plasmas 4

  7. Mechanisms of B cell Synapse Formation Predicted by Stochastic Simulation

    E-Print Network [OSTI]

    Philippos K. Tsourkas; Nicole Baumgarth; Scott I. Simon; Subhadip Raychaudhuri

    2006-10-19

    The clustering of B cell receptor (BCR) molecules and the formation of the protein segregation structure known as the immunological synapse appears to precede antigen (Ag) uptake by B cells. The mature B cell synapse is characterized by a central cluster of BCR/Ag molecular complexes surrounded by a ring of LFA-1/ICAM-1 complexes. Recent experimental evidence shows receptor clustering in B cells can occur via mechanical or signaling-driven processes. An alternative mechanism of diffusion and affinity-dependent binding has been proposed to explain synapse formation in the absence of signaling-driven processes. In this work, we investigated the biophysical mechanisms that drive immunological synapse formation in B cells across the physiological range of BCR affinity (KA~10^6-10^10 M-1) through computational modeling. Our computational approach is based on stochastic simulation of diffusion and reaction events with a clearly defined mapping between probabilistic parameters of our model and their physical equivalents. We show that a diffusion-and-binding mechanism is sufficient to drive synapse formation only at low BCR affinity and for a relatively stiff B cell membrane that undergoes little deformation. We thus predict the need for alternative mechanisms: a difference in the mechanical properties of BCR/Ag and LFA-1/ICAM-1 bonds and/or signaling driven processes.

  8. Segue 1 - A Compressed Star Formation History Before Reionization

    E-Print Network [OSTI]

    Webster, David; Bland-Hawthorn, Joss

    2015-01-01

    Segue 1 is the current best candidate for a "first galaxy", a system which experienced only a single short burst of star formation and has since remained unchanged. Here we present possible star formation scenarios which can explain its unique metallicity distribution. While the majority of stars in all other ultra-faint dwarfs (UFDs) are within 0.5 dex of the mean [Fe/H] for the galaxy, 5 of the 7 stars in Segue 1 have a spread of $\\Delta$[Fe/H] $>0.8$ dex. We show that this distribution of metallicities canot be explained by a gradual build-up of stars, but instead requires clustered star formation. Chemical tagging allows the separate unresolved delta functions in abundance space to be associated with discrete events in space and time. This provides an opportunity to put the enrichment events into a time sequence and unravel the history of the system. We investigate two possible scenarios for the star formation history of Segue 1 using Fyris Alpha simulations of gas in a $10^7$ M$_\\odot$ dark matter halo. ...

  9. Exotherm data acquisition in polyurethane foam formation using a microcomputer

    SciTech Connect (OSTI)

    Hebrard, M.J.; Leroux, J.

    1986-01-01

    An Apple microcomputer was used to collect exotherm data of the reactions leading to the formation of polyurethane foams, to differentiate the curves with respect to time and to measure the position and magnitude of the inflection points. Hardware, software, operations and reproducibility of this automated data acquisition system are described.

  10. Brown Dwarf Formation from Disk Fragmentation and Ejection

    E-Print Network [OSTI]

    Joergens, Viki

    irradiation flux 4 r midplane optical depth opacity from Bell & Lin (1990); = 2 + 20tan /3 u u ; , , / 2 , irr & Basu (2006, ApJ, 650, 956) Clump formation (gravitational instability) and migration Long;Migrating Embryo (ME) Scenario Clumps form in outer disk, radius ~ 50 ­ 100 AU, migrate inward (migration

  11. FORMATION OF ROLL WAVES IN LAMINAR SHEET FLOW

    E-Print Network [OSTI]

    Julien, Pierre Y.

    FORMATION OF ROLL WAVES IN LAMINAR SHEET FLOW by Pierre Y. Julien and David M. Hartley January 1985 . . . . . . . . . . . . . . . . . . . . . . . . . 1 I1. THEORY ON THE STABILITY OF LAMINAR SHEET FLOW . . . . . . . . . 3 2.1 Steady uniform laminar of the Coefficients fj and y for Laminar Sheet Flow . . . . . . . . . . . . . . 26 APPENDIX I1 .Experimental Data

  12. On flame kernel formation and propagation in premixed gases

    SciTech Connect (OSTI)

    Eisazadeh-Far, Kian; Metghalchi, Hameed [Northeastern University, Mechanical and Industrial Engineering Department, Boston, MA 02115 (United States); Parsinejad, Farzan [Chevron Oronite Company LLC, Richmond, CA 94801 (United States); Keck, James C. [Massachusetts Institute of Technology, Cambridge, MA 02139 (United States)

    2010-12-15

    Flame kernel formation and propagation in premixed gases have been studied experimentally and theoretically. The experiments have been carried out at constant pressure and temperature in a constant volume vessel located in a high speed shadowgraph system. The formation and propagation of the hot plasma kernel has been simulated for inert gas mixtures using a thermodynamic model. The effects of various parameters including the discharge energy, radiation losses, initial temperature and initial volume of the plasma have been studied in detail. The experiments have been extended to flame kernel formation and propagation of methane/air mixtures. The effect of energy terms including spark energy, chemical energy and energy losses on flame kernel formation and propagation have been investigated. The inputs for this model are the initial conditions of the mixture and experimental data for flame radii. It is concluded that these are the most important parameters effecting plasma kernel growth. The results of laminar burning speeds have been compared with previously published results and are in good agreement. (author)

  13. Star Formation Activity in CLASH Brightest Cluster Galaxies

    E-Print Network [OSTI]

    Fogarty, Kevin; Connor, Thomas; Donahue, Megan; Moustakas, John

    2015-01-01

    The CLASH X-ray selected sample of 20 galaxy clusters contains ten brightest cluster galaxies (BCGs) that exhibit significant ($>$5 $\\sigma$) extinction-corrected star formation rates (SFRs). Star formation activity is inferred from photometric estimates of UV and H$\\alpha$+[NII] emission in knots and filaments detected in CLASH HST observations. These measurements are supplemented with [OII], [OIII], and H$\\beta$ fluxes measured from spectra obtained with the SOAR telescope. Reddening-corrected UV-derived SFRs in these BCGs are broadly consistent with H$\\alpha$-derived SFRs. Five BCGs exhibit SFRs $>$10 M$_{\\odot}$ yr$^{-1}$ and an additional two have a SFR $>$ 100 M$_{\\odot}$ yr$^{-1}$. We confirm that photoionization from ongoing star formation powers the line emission nebulae in these BCGs, although in many BCGs there is also evidence for a LINER-like contribution. Using Chandra X-ray measurements, we infer that the star formation occurs exclusively in low-entropy cluster cores and exhibits a correlation ...

  14. GDCT Initialization File [gdct.ini] Format Specification Guide

    E-Print Network [OSTI]

    Rosebrugh, Robert

    GDCT Initialization File [gdct.ini] Format Specification Guide Written By: Jeremy Bradbury June 22, 2000 Below is the layout of the gdct.ini file. It is important to note the following: · If the gdct.ini to represent that a file does not exist under the "Recent Files" section of the gdct.ini file. [Internal

  15. Star Formation and the ISM in Four Dwarf Irregular Galaxies

    E-Print Network [OSTI]

    L. M. Young; L. van Zee; K. Y. Lo; R. C. Dohm-Palmer; M. E. Beierle

    2003-04-14

    We present new, high sensitivity VLA observations of HI in four dwarf galaxies (UGCA 292, GR8, DDO 210, and DDO 216) and we use these data to study interactions between star formation and the interstellar medium. HI velocity dispersions and line shapes in UGCA 292, GR8, and DDO 210 show that these three galaxies contain both warm and cool or cold HI phases. The presence of the cold neutral medium is indicated by a low-dispersion (3--6 km/s) HI component or by the Gauss-Hermite shape parameter h_4 > 0. Contrary to expectations, we find no trend between the incidence of the low-dispersion (colder) phase and the star formation rate in five dwarf galaxies. The colder HI phase may be a necessary ingredient for star formation, but it is clearly not sufficient. However, there is a global trend between the star formation rate of a galaxy and the incidence of asymmetric HI profiles. This trend probably reflects kinetic energy input from young massive stars. Numerical simulations show that the effects of rotational broadening (finite angular resolution) are minimal for these galaxies. Simulations are also used to estimate the errors in the column densities of the high-dispersion and the low-dispersion HI phases.

  16. Star formation in the merging galaxy cluster Abell 3921

    E-Print Network [OSTI]

    C. Ferrari; S. Maurogordato; L. Feretti; R. W. Hunstead; C. Benoist; A. Cappi; S. Schindler; E. Slezak

    2005-10-04

    Through a combined optical and radio analysis, we have investigated the possible connection between the dynamical state of the merging cluster A3921 and its star formation properties, reaching the conclusion that the on-going merger is triggering a SF episode in the collision region.

  17. Star formation in the merging galaxy cluster Abell 3921

    E-Print Network [OSTI]

    Ferrari, C; Feretti, L; Hunstead, R W; Benoist, C; Cappi, A; Schindler, S; Slezak, E

    2005-01-01

    Through a combined optical and radio analysis, we have investigated the possible connection between the dynamical state of the merging cluster A3921 and its star formation properties, reaching the conclusion that the on-going merger is triggering a SF episode in the collision region.

  18. A Review of Impending Small Satellite Formation Flying Missions

    E-Print Network [OSTI]

    Chung, Soon-Jo

    A Review of Impending Small Satellite Formation Flying Missions Saptarshi Bandyopadhyay , Giri P. Subramanian , Rebecca Foust , Daniel Morgan§ , Soon-Jo Chung¶ , University of Illinois at Urbana-Champaign, Urbana, Illinois, 61801, USA and Fred Y. Hadaegh Jet Propulsion Laboratory, California Institute

  19. CORONAL WAVES, SHOCK FORMATION AND CORONAL MASS Received: . . . . . . ; Accepted: . . . . . .

    E-Print Network [OSTI]

    Hudson, Hugh

    waves was recognized early from the radio type II bursts, for which the high brightness temperaturesCORONAL WAVES, SHOCK FORMATION AND CORONAL MASS EJECTIONS Received: . . . . . . ; Accepted: . . . . . . Table of Contents 1 Shocks, blast waves, piston driven shocks 2 2 Identification of coronal waves 3 3

  20. Kinetic model for nitric oxide formation during pulverized coal combustion

    SciTech Connect (OSTI)

    Mitchell, J.W.; Tarbell, J.M.

    1982-03-01

    A mathematical model of NO formation during pulverised coal combustion was developed from a proposed kinetic mechanism involving 12 overall chemical reactions. Most significantly, the model describes the complex conversion of coal bound nitrogen compounds to NO during combustion. The predictions of the model compare favourably with literature data and are in qualitative agreement with trends observed in practical coal combustion.

  1. Wave optics and image formation in gravitational lensing

    E-Print Network [OSTI]

    Yasusada Nambu

    2012-07-30

    We discuss image formation in gravitational lensing systems using wave optics. Applying the Fresnel-Kirchhoff diffraction formula to waves scattered by a gravitational potential of a lens object, we demonstrate how images of source objects are obtained directly from wave functions without using a lens equation for gravitational lensing.

  2. (Sub)mm Interferometry Applications in Star Formation Research

    E-Print Network [OSTI]

    Beuther, Henrik

    (Sub)mm Interferometry Applications in Star Formation Research H. Beuther1 Max-Planck Institute for Astronomy, K¨onigstuhl 17, 69117 Heidelberg, Germany beuther@mpia.de Abstract. Interferometry at (sub)mm structure e.g. details of accretion disks or molecular outflows and the sub(mm) wavelength bands

  3. Analysis of Star Formation in Galaxy-like Objects

    E-Print Network [OSTI]

    Patricia B. Tissera

    1999-12-20

    Using cosmological hydrodynamical simulations, we investigate the effects of hierarchical aggregation on the triggering of star formation in galactic-like objects. We include a simple star formation model to transform the cold gas in dense regions into stars. Simulations with different parameters have been performed in order to quantify the dependence of the results on the parameters. We then resort to stellar population synthesis models to trace the color evolution of each object with red-shift and in relation to their merger histories. We find that, in a hierarchical clustering scenario, the process of assembling of the structure is one natural mechanism that may trigger star formation. The resulting star formation rate history for each individual galactic object is composed of a continuous one ($\\leq 3 \\rm{M_{\\odot}/yr}$) and a series of star bursts. We find that even the accretion of a small satellite can be correlated with a stellar burst. Massive mergers are found to be more efficient at transforming gas into stars

  4. Mergers and star formation in SPH cosmological simulations

    E-Print Network [OSTI]

    Patricia B. Tissera

    1999-11-02

    The star formation rate history of galactic objects in hydrodynamical cosmological simulations are analyzed in relation to their merger histories. The findings suggest that massive mergers produce more efficient starbursts and that, depending on the internal structure of the objects, double starbursts could also occur.

  5. On the Endogenous Formation of Energy Efficient Cooperative Wireless Networks

    E-Print Network [OSTI]

    Brown III, Donald R.

    On the Endogenous Formation of Energy Efficient Cooperative Wireless Networks Fatemeh Fazel and D nodes can be used as cooperative relays to reduce the transmission energy required to reliably deliver and cooperative pairings can be assigned to optimize the overall energy efficiency of the network. In networks

  6. Geomechanical Study of Bakken Formation for Improved Oil Recovery

    SciTech Connect (OSTI)

    Ling, Kegang; Zeng, Zhengwen; He, Jun; Pei, Peng; Zhou, Xuejun; Liu, Hong; Huang, Luke; Ostadhassan, Mehdi; Jabbari, Hadi; Blanksma, Derrick; Feilen, Harry; Ahmed, Salowah; Benson, Steve; Mann, Michael; LeFever, Richard; Gosnold, Will

    2013-12-31

    On October 1, 2008 US DOE-sponsored research project entitled “Geomechanical Study of Bakken Formation for Improved Oil Recovery” under agreement DE-FC26-08NT0005643 officially started at The University of North Dakota (UND). This is the final report of the project; it covers the work performed during the project period of October 1, 2008 to December 31, 2013. The objectives of this project are to outline the methodology proposed to determine the in-situ stress field and geomechanical properties of the Bakken Formation in Williston Basin, North Dakota, USA to increase the success rate of horizontal drilling and hydraulic fracturing so as to improve the recovery factor of this unconventional crude oil resource from the current 3% to a higher level. The success of horizontal drilling and hydraulic fracturing depends on knowing local in-situ stress and geomechanical properties of the rocks. We propose a proactive approach to determine the in-situ stress and related geomechanical properties of the Bakken Formation in representative areas through integrated analysis of field and well data, core sample and lab experiments. Geomechanical properties are measured by AutoLab 1500 geomechanics testing system. By integrating lab testing, core observation, numerical simulation, well log and seismic image, drilling, completion, stimulation, and production data, in-situ stresses of Bakken formation are generated. These in-situ stress maps can be used as a guideline for future horizontal drilling and multi-stage fracturing design to improve the recovery of Bakken unconventional oil.

  7. Organic Aerosol Formation Downwind from the Deepwater Horizon Oil Spill

    E-Print Network [OSTI]

    Toohey, Darin W.

    Organic Aerosol Formation Downwind from the Deepwater Horizon Oil Spill Nicole ONeill - ATOC 3500 and aerosol composition of air over the Deepwater Horizon oil spill in the Gulf of Mexico. · The lightest chemicals in the oil evaporated within hours, as scientists expected them to do. What they didn't expect

  8. DAMAGE AND ROCKVOLATILE MIXTURE EFFECTS ON IMPACT CRATER FORMATION

    E-Print Network [OSTI]

    Stewart, Sarah T.

    DAMAGE AND ROCK­VOLATILE MIXTURE EFFECTS ON IMPACT CRATER FORMATION JOHN D. O'KEEFE, SARAH T models for material damage, dilatancy, and inhomogeneous materials (mixtures). We found that a strength degradation (damage) model was necessary to produce faulting in homogeneous materials. Both normal and thrust

  9. Metal-Poor Globular Clusters and Galaxy Formation

    E-Print Network [OSTI]

    Jay Strader; Jean P. Brodie; Duncan A. Forbes

    2004-03-05

    We demonstrate a significant (> 5-sigma) correlation between the mean color of metal-poor globular cluster (GC) systems and parent galaxy luminosity. A Bayesian Markov Chain Monte Carlo method is introduced to find the mean color, and is easily generalizable to quantify multimodality in other astronomical datasets. We derive a GC color--galaxy luminosity relation of the form Z ~ L^ (0.15 +/- 0.03). When combined with evidence against a single primordial GC metallicity--galaxy luminosity relation for protogalactic fragments, the existence of such a correlation is evidence against both accretion and major merger scenarios as an explanation of the entire metal-poor GC systems of luminous galaxies. However, our relation arises naturally in an in situ picture of GC formation, and is consistent with the truncation of metal-poor GC formation by reionization. A further implication is that the ages of metal-poor GCs in dwarf galaxies constrain the main epoch of galaxy formation in hierarchical models. If the ages of old metal-poor GCs in Local Group dwarfs (> 11 Gyr) are typical of those in dwarfs elsewhere, then the bulk of galaxy assembly (at least in clusters and groups) must have occurred at z > 2.5, contrary to the predictions of some structure formation models.

  10. Composition and Formation of the Saccharomyces cerevisiae Centromeric Nucleosome

    E-Print Network [OSTI]

    Camahort, Raymond Anthony

    2008-01-01

    on these findings, we hypothesize that Scm3 is a novel yeast inner kinetochore protein that functions in the formation and maintenance of a segregation competent kinetochore through recruitment of the Cse4 octameric nucleosome. 5 TABLE OF CONTENTS............................................................................................................................5 Table of Contents.........................................................................................................6 List of Figures...

  11. NITROGEN EVOLUTION AND SOOT FORMATION DURING SECONDARY COAL PYROLYSIS

    E-Print Network [OSTI]

    Fletcher, Thomas H.

    NITROGEN EVOLUTION AND SOOT FORMATION DURING SECONDARY COAL PYROLYSIS by Haifeng Zhang DURING SECONDARY COAL PYROLYSIS Haifeng Zhang Department of Chemical Engineering Doctor of Philosophy evidence of ring opening reactions was observed during the pyrolysis of pyrene. A simple model was devised

  12. Path Planning for Permutation-Invariant Multi-Robot Formations

    E-Print Network [OSTI]

    Hutchinson, Seth

    Path Planning for Permutation-Invariant Multi-Robot Formations Stephen Kloder Seth Hutchinson, IL 61801 Email: {kloder, seth}@uiuc.edu Abstract-- In this paper we demonstrate path planning for our-assign roles for each individual robot, rely on local planning and behaviors to build emergent behaviors

  13. Formation of Iron Nanoparticles and Increase in Iron Reactivity in

    E-Print Network [OSTI]

    Benning, Liane G.

    each on presieved (goethite suspensions. Microscopic analyses of the processed soil and goethite samples reveal the neo-formation of Fe-rich nanoparticle aggregates, which were(III) oxide (mainly goethite or hematite) and clay minerals. At circumneutral pH, the solubility of Fe

  14. A simple model of the hierarchical formation of galaxies

    E-Print Network [OSTI]

    B. Hoeneisen

    2000-09-05

    We develop a simple, fast and predictive model of the hierarchical formation of galaxies which is in quantitative agreement with observations. Comparing simulations with observations we place constraints on the density of the universe and on the power spectrum of density fluctuations.

  15. PROMINENCE FORMATION ASSOCIATED WITH AN EMERGING HELICAL FLUX ROPE

    SciTech Connect (OSTI)

    Okamoto, Takenori J.; Tsuneta, Saku; Katsukawa, Yukio; Suematsu, Yoshinori [National Astronomical Observatory, Mitaka, Tokyo, 181-8588 (Japan); Lites, Bruce W.; Kubo, Masahito [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000 (United States); Yokoyama, Takaaki [Department of Earth and Planetary Science, School of Science, University of Tokyo, Hongo, Bunkyo, Tokyo, 113-0033 (Japan); Berger, Thomas E.; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M. [Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover St., Palo Alto, CA 94304 (United States); Ichimoto, Kiyoshi; Nagata, Shin'ichi; Shibata, Kazunari [Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto, 607-8471 (Japan); Shimizu, Toshifumi [ISAS/JAXA, Sagamihara, Kanagawa, 229-8510 (Japan)], E-mail: joten.okamoto@nao.ac.jp

    2009-05-20

    The formation and evolution process and magnetic configuration of solar prominences remain unclear. In order to study the formation process of prominences, we examine continuous observations of a prominence in NOAA AR 10953 with the Solar Optical Telescope on the Hinode satellite. As reported in our previous Letter, we find a signature suggesting that a helical flux rope emerges from below the photosphere under a pre-existing prominence. Here we investigate more detailed properties and photospheric indications of the emerging helical flux rope, and discuss their relationship to the formation of the prominence. Our main conclusions are: (1) a dark region with absence of strong vertical magnetic fields broadens and then narrows in Ca II H-line filtergrams. This phenomenon is consistent with the emergence of the helical flux rope as photospheric counterparts. The size of the flux rope is roughly 30,000 km long and 10,000 km wide. The width is larger than that of the prominence. (2) No shear motion or converging flows are detected, but we find diverging flows such as mesogranules along the polarity inversion line. The presence of mesogranules may be related to the emergence of the helical flux rope. (3) The emerging helical flux rope reconnects with magnetic fields of the pre-existing prominence to stabilize the prominence for the next several days. We thus conjecture that prominence coronal magnetic fields emerge in the form of helical flux ropes that contribute to the formation and maintenance of the prominence.

  16. Graphene defect formation by extreme ultraviolet generated photoelectrons

    SciTech Connect (OSTI)

    Gao, A., E-mail: a.gao@utwente.nl; Lee, C. J.; Bijkerk, F. [FOM-Dutch Institute for Fundamental Energy Research, Edisonbaan 14, 3439 MN Nieuwegein, The Netherlands and XUV Optics Group, MESA Institute for Nanotechnology, University of Twente, P.O. Box 217, 7500 AE, Enschede (Netherlands)

    2014-08-07

    We have studied the effect of photoelectrons on defect formation in graphene during extreme ultraviolet (EUV) irradiation. Assuming the major role of these low energy electrons, we have mimicked the process by using low energy primary electrons. Graphene is irradiated by an electron beam with energy lower than 80?eV. After e-beam irradiation, it is found that the D peak, I(D), appears in the Raman spectrum, indicating defect formation in graphene. The evolution of I(D)/I(G) follows the amorphization trajectory with increasing irradiation dose, indicating that graphene goes through a transformation from microcrystalline to nanocrystalline and then further to amorphous carbon. Further, irradiation of graphene with increased water partial pressure does not significantly change the Raman spectra, which suggests that, in the extremely low energy range, e-beam induced chemical reactions between residual water and graphene are not the dominant mechanism driving defect formation in graphene. Single layer graphene, partially suspended over holes was irradiated with EUV radiation. By comparing with the Raman results from e-beam irradiation, it is concluded that the photoelectrons, especially those from the valence band, contribute to defect formation in graphene during irradiation.

  17. On formation of equation of state of evolving quantum field

    E-Print Network [OSTI]

    A. V. Leonidov; A. A. Radovskaya

    2014-12-13

    Stylized model of evolution of matter created in ultra relativistic heavy ion collisions is considered. Systematic procedure of computing quantum corrections in the framework of Keldysh formalism is formulated. Analytical expressions for formation of equations of state taking into account leading quantum corrections is worked out, complete description of subleasing corrections and analytical expressions for some of them is presented.

  18. Mineral formation during simulated leaks of Hanford waste tanks

    E-Print Network [OSTI]

    Flury, Markus

    Mineral formation during simulated leaks of Hanford waste tanks Youjun Deng a , James B. Harsh a at the US DOE Hanford Site, Washington, caus- ing mineral dissolution and re-precipitation upon contact with subsurface sediments. The main mineral precipitation and transformation pathways were studied in solutions

  19. Predicting Nickel Precipitate Formation in Contaminated Soils. (3717)

    E-Print Network [OSTI]

    Sparks, Donald L.

    Predicting Nickel Precipitate Formation in Contaminated Soils. (3717) Authors: E. Peltier* - Univ in contaminated soils plays a crucial role in determining the long term fate of toxic metal pollutants speciation in laboratory contaminated soils with thermodynamic and kinetic analyses of precipitate stability

  20. Thermally Triggered Calcium Phosphate Formation from Calcium-Loaded Liposomes

    E-Print Network [OSTI]

    of utilizing lipid vesicles for the synthesis of inorganic solids of controlled shape and/or size is well the rapid in situ formation of polymer hydrogels, inorganic solids, and other materials for medical. Mixing of a calcium-loaded lipid vesicle suspension with aqueous inorganic phosphate resulted in a stable

  1. Quantum origin of an anomalous isotope effect in ozone formation

    E-Print Network [OSTI]

    Reid, Scott A.

    Quantum origin of an anomalous isotope effect in ozone formation D. Babikov *, B.K. Kendrick, R mechanical calculations of the ðJ ¼ 0Þ energies and lifetimes of the metastable states of ozone on a new effect in the reaction that forms ozone because of their role in the energy transfer mechanism, in which

  2. One Nanometer Resolution Electrical Probe via Atomic Metal Filament Formation

    E-Print Network [OSTI]

    Cui, Yi

    One Nanometer Resolution Electrical Probe via Atomic Metal Filament Formation Seung Sae Hong, Judy an atomic-size metallic filament on a commercial C-AFM tip. We demonstrate 1 nm lateral resolution in C-AFM using the metal filament tip. The filament tip is mechanically robust and electrically stable

  3. Viscoelastic damage modeling of sinkhole formation Eyal Shalev*, Vladimir Lyakhovsky

    E-Print Network [OSTI]

    Lyakhovsky, Vladimir

    Viscoelastic damage modeling of sinkhole formation Eyal Shalev*, Vladimir Lyakhovsky Geological 2012 Keywords: Sinkholes Damage Viscoelasticity Modeling a b s t r a c t The sinkholes along the Dead Sea coast are observed in two main sedimentary environments: alluvial fan sinkholes, which usually

  4. Nonequilibrium pattern formation and spatiotemporal chaos in fluid convection

    SciTech Connect (OSTI)

    Michael Cross

    2006-09-13

    The final report for grant number DE-FG03-98ER14891 summarizes the application of the unique simulation capabilities developed under DOE support to investigations of important issues in pattern formation and spatiotemporal chaos in Rayleigh-Benard convection, particularly emphasizing quantitative contact with the active experimental programs.

  5. A PROBABILISTIC FINITE ELEMENT ANALYSIS OF RESIDUAL STRESS FORMATION

    E-Print Network [OSTI]

    Grujicic, Mica

    A PROBABILISTIC FINITE ELEMENT ANALYSIS OF RESIDUAL STRESS FORMATION IN SHRINK-FIT CERAMIC shrink fitting of the jacket over the lining is studied using a probabilistic finite element analysis structural analysis approach, known as the Advanced Mean Value (AMV) method, is used which enables

  6. Structure formation in the presence of dark energy perturbations

    E-Print Network [OSTI]

    L. R. Abramo; R. C. Batista; L. Liberato; R. Rosenfeld

    2007-11-28

    We study non-linear structure formation in the presence of dark energy. The influence of dark energy on the growth of large-scale cosmological structures is exerted both through its background effect on the expansion rate, and through its perturbations as well. In order to compute the rate of formation of massive objects we employ the Spherical Collapse formalism, which we generalize to include fluids with pressure. We show that the resulting non-linear evolution equations are identical to the ones obtained in the Pseudo-Newtonian approach to cosmological perturbations, in the regime where an equation of state serves to describe both the background pressure relative to density, and the pressure perturbations relative to the density perturbations as well. We then consider a wide range of constant and time-dependent equations of state (including phantom models) parametrized in a standard way, and study their impact on the non-linear growth of structure. The main effect is the formation of dark energy structure associated with the dark matter halo: non-phantom equations of state induce the formation of a dark energy halo, damping the growth of structures; phantom models, on the other hand, generate dark energy voids, enhancing structure growth. Finally, we employ the Press-Schechter formalism to compute how dark energy affects the number of massive objects as a function of redshift.

  7. Cellular pattern formation in circular domains Antonio Palacios,a)

    E-Print Network [OSTI]

    Cellular pattern formation in circular domains Antonio Palacios,a) Gemunu H. Gunaratne 1997; accepted for publication 24 June 1997 An analysis of stationary and nonstationary cellular. Motivated by the observa- tion of novel stationary and nonstationary cellular states on a flame front, we

  8. Effect of gaseous inhibitors on PCDD/F formation

    SciTech Connect (OSTI)

    Ruokojaervi, P.H.; Halonen, I.A.; Tuppurainen, K.A.; Tarhanen, J.; Ruuskanen, J.

    1998-10-15

    Emissions of polychlorinated dibenzo-p-dioxins (PCDDs) and dibenzofurans (PCDFs) from municipal waste incineration are currently a subject of considerable public concern because of their extreme toxicity. PCDD/F formation in incineration processes is being studied widely, but studies on inhibition are quite sparse, especially in a pilot-plant scale. In this work, the effect of four gaseous inhibitors (sulfur dioxide, ammonia, dimethylamine, and methyl mercaptan) on PCDD/PCDF formation in the combustion of liquid fuel was studied using a pilot-scale plant. The inhibitors were injected into the flue gas stream after the first economizer at a temperature of 670 C and just before the second economizer at 410 C. Both the chlorophenol and PCDD and PCDF concentrations decreased when inhibitors were added. Particle-phase PCDD/F concentrations in particular decreased by up to 98%. The results suggest that the formation of PCDD/Fs is hindered in the particle phase at the early stages of the PCDD/F formation chain, probably even before precursors such as chlorophenols have been formed.

  9. Formation of Secondary Containment Systems Using Permeation of Colloidal Silica

    E-Print Network [OSTI]

    Zornberg, Jorge G.

    the tanks. This study evaluates the formation of hydraulic barriers for secondary containment through the permeation of colloidal silica grout. A sim- plified infiltration model is presented to predict the downward. Because the simplified infiltration model cannot predict the soil-grout interaction or the permeation

  10. Hemodynamics Before and After Bleb Formation in Cerebral Aneurysms

    E-Print Network [OSTI]

    Frangi, Alejandro

    the intraaneurysmal hemodynamic pattern changes after bleb formation. Seven intracranial aneurysms harboring well of the vessel wall may be caused by elevated WSS associated with the inflow jet. However, the final shape the first attempt at testing this hypothesis. For this purpose, patient-specific computational fluid

  11. The formation and evolution of synthetic jets Barton L. Smitha)

    E-Print Network [OSTI]

    Smith, Barton L.

    The formation and evolution of synthetic jets Barton L. Smitha) and Ari Glezer Woodruff School 1997; accepted 6 May 1998 A nominally plane turbulent jet is synthesized by the interactions of a train of a flexible diaphragm in a sealed cavity. Even though the jet is formed without net mass injection

  12. Mesoscale simulations of surfactant dissolution and mesophase formation

    E-Print Network [OSTI]

    P. Prinsen; P. B. Warren; M. A. J. Michels

    2002-04-22

    The evolution of the contact zone between pure surfactant and solvent has been studied by mesoscale simulation. It is found that mesophase formation becomes diffusion controlled and follows the equilibrium phase diagram adiabatically almost as soon as individual mesophases can be identified, corresponding to times in real systems of order 10 microseconds.

  13. Formation of Jets by Baroclinic Turbulence BRIAN F. FARRELL

    E-Print Network [OSTI]

    Farrell, Brian F.

    Formation of Jets by Baroclinic Turbulence BRIAN F. FARRELL Department of Earth and Planetary spatial-scale jets; geophysical examples of this phenomenon include the Jovian banded winds and the earth's polar-front jet. These relatively steady large-scale jets arise from and are maintained by the smaller

  14. Hydrocarbon Formation in Metallic Iron/Water Systems

    E-Print Network [OSTI]

    Deng, Baolin

    Hydrocarbon Formation in Metallic Iron/Water Systems B A O L I N D E N G , , § T I M O T H Y J . C-labeled hydrocarbons are produced. In the absence of chlorinated ethenes, however, lower con- centrations of many of the same hydrocarbons (methane and C2-C6 alkanes and alkenes) are also produced. Hardy and Gillham (1996

  15. Implantation conditions for diamond nanocrystal formation in amorphous silica

    SciTech Connect (OSTI)

    Buljan, Maja; Radovic, Iva Bogdanovic; Desnica, Uros V.; Ivanda, Mile; Jaksic, Milko; Saguy, Cecile; Kalish, Rafi; Djerdj, Igor; Tonejc, Andelka; Gamulin, Ozren

    2008-08-01

    We present a study of carbon ion implantation in amorphous silica, which, followed by annealing in a hydrogen-rich environment, leads to preferential formation of carbon nanocrystals with cubic diamond (c-diamond), face-centered cubic (n-diamond), or simple cubic (i-carbon) carbon crystal lattices. Two different annealing treatments were used: furnace annealing for 1 h and rapid thermal annealing for a brief period, which enables monitoring of early nucleation events. The influence of implanted dose and annealing type on carbon and hydrogen concentrations, clustering, and bonding were investigated. Rutherford backscattering, elastic recoil detection analysis, infrared spectroscopy, transmission electron microscopy, selected area electron diffraction, ultraviolet-visible absorption measurements, and Raman spectroscopy were used to study these carbon formations. These results, combined with the results of previous investigations on similar systems, show that preferential formation of different carbon phases (diamond, n-diamond, or i-carbon) depends on implantation energy, implantation dose, and annealing conditions. Diamond nanocrystals formed at a relatively low carbon volume density are achieved by deeper implantation and/or lower implanted dose. Higher volume densities led to n-diamond and finally to i-carbon crystal formation. This observed behavior is related to damage sites induced by implantation. The optical properties of different carbon nanocrystal phases were significantly different.

  16. A SUMMARY OF COAL IN THE COALMONT FORMATION (TERTIARY),

    E-Print Network [OSTI]

    Chapter SN A SUMMARY OF COAL IN THE COALMONT FORMATION (TERTIARY), NORTH PARK BASIN, COLORADO By S assessment of selected Tertiary coal beds and zones in the Northern RockyMountains and Great Plains region, U Resource assessment of selected Tertiary coal beds and zones in the Northern Rocky Mountains and Great

  17. Particulate Interactions in Dry

    E-Print Network [OSTI]

    Frey, Pascal

    is available from the British Library Library of Congress Cataloging in Publication Data Zeng, Xian Ming, 1963-203-20959-1 Master e-book ISBN ISBN 0-203-26768-0 (Adobe eReader Format) #12;Contents Chapter 1 Interparticulate.3 Electrical properties 35 2.4 Water vapour condensation 37 2.5 Particle morphology 42 2.6 Polymorphism

  18. Sam Houston State University A Member of The Texas State University System

    E-Print Network [OSTI]

    Short, Jon W.

    -IR-02 SHSU Web Accessibility Sam Houston State University is committed to making all official, academic the site. Major reports and other publications that are on the Web site are generally available in HTML or Adobe Portable Document Format. SHSU is committed to making its Web site accessible according

  19. Modeling jet and outflow feedback during star cluster formation

    SciTech Connect (OSTI)

    Federrath, Christoph; Schrön, Martin; Banerjee, Robi; Klessen, Ralf S.

    2014-08-01

    Powerful jets and outflows are launched from the protostellar disks around newborn stars. These outflows carry enough mass and momentum to transform the structure of their parent molecular cloud and to potentially control star formation itself. Despite their importance, we have not been able to fully quantify the impact of jets and outflows during the formation of a star cluster. The main problem lies in limited computing power. We would have to resolve the magnetic jet-launching mechanism close to the protostar and at the same time follow the evolution of a parsec-size cloud for a million years. Current computer power and codes fall orders of magnitude short of achieving this. In order to overcome this problem, we implement a subgrid-scale (SGS) model for launching jets and outflows, which demonstrably converges and reproduces the mass, linear and angular momentum transfer, and the speed of real jets, with ?1000 times lower resolution than would be required without the SGS model. We apply the new SGS model to turbulent, magnetized star cluster formation and show that jets and outflows (1) eject about one-fourth of their parent molecular clump in high-speed jets, quickly reaching distances of more than a parsec, (2) reduce the star formation rate by about a factor of two, and (3) lead to the formation of ?1.5 times as many stars compared to the no-outflow case. Most importantly, we find that jets and outflows reduce the average star mass by a factor of ? three and may thus be essential for understanding the characteristic mass of the stellar initial mass function.

  20. Energetics of Swimming and Flying in Formation Formation movement during swimming and flying has been hypothesized to reduce

    E-Print Network [OSTI]

    Fish, Frank

    been hypothesized to reduce an individual animal's energy expenditure. Individuals in a formation by vorticity shed from leading animals can be used to lowerthe drag and energy expenditure ontrailing energy savings in fish schools is a diamond shape. Vorticity shed from rigid bodies, such as cars

  1. Soot formation in diesel combustion under high-EGR conditions.

    SciTech Connect (OSTI)

    Idicheria, Cherian A.; Pickett, Lyle M.

    2005-06-01

    Experiments were conducted in an optically accessible constant-volume combustion vessel to investigate soot formation at diesel combustion conditions - in a high exhaust-gas recirculation (EGR) environment. The ambient oxygen concentration was decreased systematically from 21% to 8% to simulate a wide range of EGR conditions. Quantitative measurements of in-situ soot in quasi-steady n-heptane and No.2 diesel fuel jets were made by using laser extinction and planar laser-induced incandescence (PLII) measurements. Flame lift-off length measurements were also made in support of the soot measurements. At constant ambient temperature, results show that the equivalence ratio estimated at the lift-off length does not vary with the use of EGR, implying an equal amount of fuel-air mixing prior to combustion. Soot measurements show that the soot volume fraction decreases with increasing EGR. The regions of soot formation are effectively 'stretched out' to longer axial and radial distances from the injector with increasing EGR, according to the dilution in ambient oxygen. However, the axial soot distribution and location of maximum soot collapses if plotted in terms of a 'flame coordinate', where the relative fuel-oxygen mixture is equivalent. The total soot in the jet cross-section at the maximum axial soot location initially increases and then decreases to zero as the oxygen concentration decreases from 21% to 8%. The trend is caused by competition between soot formation rates and increasing residence time. Soot formation rates decrease with decreasing oxygen concentration because of the lower combustion temperatures. At the same time, the residence time for soot formation increases, allowing more time for accumulation of soot. Increasing the ambient temperature above nominal diesel engine conditions leads to a rapid increase in soot for high-EGR conditions when compared to conditions with no EGR. This result emphasizes the importance of EGR cooling and its beneficial effect on mitigating soot formation. The effect of EGR is consistent for different fuels but soot levels depend on the sooting propensity of the fuel. Specifically, No.2 diesel fuel produces soot levels more than ten times higher than those of n-heptane.

  2. Controlling and assessing pressure conditions during treatment of tar sands formations

    SciTech Connect (OSTI)

    Zhang, Etuan; Beer, Gary Lee

    2015-11-10

    A method for treating a tar sands formation includes providing heat to at least part of a hydrocarbon layer in the tar sands formation from a plurality of heaters located in the formation. Heat is allowed to transfer from the heaters to at least a portion of the formation. A pressure in the portion of the formation is controlled such that the pressure remains below a fracture pressure of the formation overburden while allowing the portion of the formation to heat to a selected average temperature of at least about 280.degree. C. and at most about 300.degree. C. The pressure in the portion of the formation is reduced to a selected pressure after the portion of the formation reaches the selected average temperature.

  3. The Death Star Migration is a practice-as-research project exploring concepts of human-to-place relationships and embodied wilderness

    E-Print Network [OSTI]

    Hernes, Peter J.

    aerial apparatus, acrobatic stilts and infused ritual and Butoh influenced movement works. She also works

  4. A General Systems Theory for Rain Formation in Warm Clouds

    E-Print Network [OSTI]

    A. M. Selvam

    2014-08-15

    A cumulus cloud model which can explain the observed characteristics of warm rain formation in monsoon clouds is presented. The model is based on classical statistical physical concepts and satisfies the principle of maximum entropy production. Atmospheric flows exhibit selfsimilar fractal fluctuations that are ubiquitous to all dynamical systems in nature, such as physical, chemical, social, etc and are characterized by inverse power law form for power (eddy energy) spectrum signifying long-range space-time correlations. A general systems theory model for atmospheric flows developed by the author is based on the concept that the large eddy energy is the integrated mean of enclosed turbulent (small scale) eddies. This model gives scale-free universal governing equations for cloud growth processes. The model predicted cloud parameters are in agreement with reported observations, in particular, the cloud dropsize distribution. Rain formation can occur in warm clouds within 30minutes lifetime under favourable conditions of moisture supply in the environment.

  5. Why are Halo Density Profiles Stable at Formation?

    E-Print Network [OSTI]

    G. Gonzalez-Casado; A. Raig; E. Salvador-Sole

    1998-10-28

    We analyze the physical justification of the picture proposed by Salvador-Sole et al. in these proceedings for the time evolution of the universal density profile of dark-matter halos. According to this picture, halos have at formation a stable (i.e. independent of mass and time) dimensionless density profile, the characteristic length and density scales of the profile depending on the underlying cosmogony. Subsequent evolution is driven by mass accretion onto the outskirts of halos and can be characterized simply by the increment of halo radius with time and the corresponding decrease of the critical density of the universe. We find this picture to be a reasonable good description of the expected evolution of halos in hierarchical models of structure formation.

  6. Role of nucleation sites on the formation of nanoporous Ge

    SciTech Connect (OSTI)

    Yates, B. R.; Darby, B. L.; Jones, K. S. [Department of Materials Science and Engineering, University of Florida, Gainesville, Florida 32611-6400 (United States); Elliman, R. G. [Department of Electronic Materials Engineering, Research School of Physical Sciences and Engineering, Australian National University, Canberra, Australian Capital Territory 0200 (Australia)

    2012-09-24

    The role of nucleation sites on the formation of nanoporous Ge was investigated. Three Ge films with different spherical or columnar pore morphologies to act as inherent nucleation sites were sputtered on (001) Ge. Samples were implanted 90 Degree-Sign from incidence at 300 keV with fluences ranging from 3.0 Multiplication-Sign 10{sup 15} to 3.0 Multiplication-Sign 10{sup 16} Ge{sup +}/cm{sup 2}. Electron microscopy investigations revealed varying thresholds for nanoporous Ge formation and exhibited a stark difference in the evolution of the Ge layers based on the microstructure of the initial film. The results suggest that the presence of inherent nucleation sites significantly alters the onset and evolution of nanoporous Ge.

  7. Exploitation and Optimization of Reservoir Performance in Hunton Formation, Oklahoma

    SciTech Connect (OSTI)

    Mohan Kelkar

    2007-06-30

    Hunton formation in Oklahoma has been the subject of attention for the last ten years. The new interest started with the drilling of the West Carney field in 1995 in Lincoln County. Subsequently, many other operators have expanded the search for oil and gas in Hunton formation in other parts of Oklahoma. These fields exhibit many unique production characteristics, including: (1) decreasing water-oil or water-gas ratio over time; (2) decreasing gas-oil ratio followed by an increase; (3) poor prediction capability of the reserves based on the log data; and (4) low geological connectivity but high hydrodynamic connectivity. The purpose of this investigation is to understand the principal mechanisms affecting the production, and propose methods by which we can optimize the production from fields with similar characteristics.

  8. Instability of black hole formation in gravitational collapse

    SciTech Connect (OSTI)

    Joshi, Pankaj S.; Malafarina, Daniele

    2011-01-15

    We consider here the classic scenario given by Oppenheimer, Snyder, and Datt, for the gravitational collapse of a massive matter cloud, and examine its stability under the introduction of small tangential stresses. We show, by offering an explicit class of physically valid tangential stress perturbations, that an introduction of tangential pressure, however small, can qualitatively change the final fate of collapse from a black hole final state to a naked singularity. This shows instability of black hole formation in collapse and sheds important light on the nature of cosmic censorship hypothesis and its possible formulations. The key effect of these perturbations is to alter the trapped surface formation pattern within the collapsing cloud and the apparent horizon structure. This allows the singularity to be visible, and implications are discussed.

  9. Structure formation in modified gravity models alternative to dark energy

    E-Print Network [OSTI]

    Kazuya Koyama

    2006-01-10

    We study structure formation in phenomenological models in which the Friedmann equation receives a correction of the form $H^{\\alpha}/r_c^{2-\\alpha}$, which realize an accelerated expansion without dark energy. In order to address structure formation in these model, we construct simple covariant gravitational equations which give the modified Friedmann equation with $\\alpha=2/n$ where $n$ is an integer. For $n=2$, the underlying theory is known as a 5D braneworld model (the DGP model). Thus the models interpolate between the DGP model ($n=2, \\alpha=1$) and the LCDM model in general relativity ($n \\to \\infty, \\alpha \\to 0$). Using the covariant equations, cosmological perturbations are analyzed. It is shown that in order to satisfy the Bianchi identity at a perturbative level, we need to introduce a correction term $E_{\\mu \

  10. Structure formation in modified gravity models alternative to dark energy

    E-Print Network [OSTI]

    Koyama, K

    2006-01-01

    We study structure formation in phenomenological models in which the Friedmann equation receives a correction of the form $H^{\\alpha}/r_c^{2-\\alpha}$, which realize an accelerated expansion without dark energy. In order to address structure formation in these model, we construct simple covariant gravitational equations which give the modified Friedmann equation with $\\alpha=2/n$ where $n$ is an integer. For $n=2$, the underlying theory is known as a 5D braneworld model (the DGP model). Thus the models interpolate between the DGP model ($n=2, \\alpha=1$) and the LCDM model in general relativity ($n \\to \\infty, \\alpha \\to 0$). Using the covariant equations, cosmological perturbations are analyzed. It is shown that in order to satisfy the Bianchi identity at a perturbative level, we need to introduce a correction term $E_{\\mu \

  11. PROTOSTELLAR DISK FORMATION ENABLED BY WEAK, MISALIGNED MAGNETIC FIELDS

    SciTech Connect (OSTI)

    Krumholz, Mark R.; Crutcher, Richard M.; Hull, Charles L. H.

    2013-04-10

    The gas from which stars form is magnetized, and strong magnetic fields can efficiently transport angular momentum. Most theoretical models of this phenomenon find that it should prevent formation of large (>100 AU), rotationally supported disks around most protostars, even when non-ideal magnetohydrodynamic (MHD) effects that allow the field and gas to decouple are taken into account. Using recent observations of magnetic field strengths and orientations in protostellar cores, we show that this conclusion is incorrect. The distribution of magnetic field strengths is very broad, and alignments between fields and angular momentum vectors within protostellar cores are essentially random. By combining the field strength and misalignment data with MHD simulations showing that disk formation is expected for both weak and misaligned fields, we show that these observations imply that we should expect disk fractions of {approx}10%-50% even when protostars are still deeply embedded in their parent cores, and even if the gas is governed by ideal MHD.

  12. Diffusive dynamics of contact formation in disordered polypeptides

    E-Print Network [OSTI]

    Gul Zerze; Jeetain Mittal; Robert B. Best

    2015-07-09

    Experiments measuring contact formation between a probe and quencher in disordered chains provide information on the fundamental dynamical timescales relevant to protein folding, but their interpretation usually relies on simplified one-dimensional (1D) diffusion models. Here, we use all-atom molecular simulations to capture both the time-scales of contact formation, as well as the scaling with the length of the peptide for tryptophan triplet quenching experiments. Capturing the experimental quenching times depends on the water viscosity, but more importantly on the configurational space explored by the chain. We also show that very similar results are obtained from Szabo-Schulten-Schulten theory applied to a 1D diffusion model derived from the simulations, supporting the validity of such models. However, we also find a significant reduction in diffusivity at small separations, those which are most important in determining the quenching rate.

  13. Diffusive dynamics of contact formation in disordered polypeptides

    E-Print Network [OSTI]

    Zerze, Gul; Best, Robert B

    2015-01-01

    Experiments measuring contact formation between a probe and quencher in disordered chains provide information on the fundamental dynamical timescales relevant to protein folding, but their interpretation usually relies on simplified one-dimensional (1D) diffusion models. Here, we use all-atom molecular simulations to capture both the time-scales of contact formation, as well as the scaling with the length of the peptide for tryptophan triplet quenching experiments. Capturing the experimental quenching times depends on the water viscosity, but more importantly on the configurational space explored by the chain. We also show that very similar results are obtained from Szabo-Schulten-Schulten theory applied to a 1D diffusion model derived from the simulations, supporting the validity of such models. However, we also find a significant reduction in diffusivity at small separations, those which are most important in determining the quenching rate.

  14. Formation of superheavy nuclei in cold fusion reactions

    E-Print Network [OSTI]

    Feng, Zhao-Qing; Li, Jun-Qing; Scheid, Werner

    2007-01-01

    Within the concept of the dinuclear system (DNS), a dynamical model is proposed for describing the formation of superheavy nuclei in complete fusion reactions by incorporating the coupling of the relative motion to the nucleon transfer process. The capture of two heavy colliding nuclei, the formation of the compound nucleus and the de-excitation process are calculated by using an empirical coupled channel model, solving a master equation numerically and applying statistical theory, respectively. Evaporation residue excitation functions in cold fusion reactions are investigated systematically and compared with available experimental data. Maximal production cross sections of superheavy nuclei in cold fusion reactions with stable neutron-rich projectiles are obtained. Isotopic trends in the production of the superheavy elements Z=110, 112, 114, 116, 118 and 120 are analyzed systematically. Optimal combinations and the corresponding excitation energies are proposed.

  15. Formation of superheavy nuclei in cold fusion reactions

    E-Print Network [OSTI]

    Zhao-Qing Feng; Gen-Ming Jin; Jun-Qing Li; Werner Scheid

    2007-10-17

    Within the concept of the dinuclear system (DNS), a dynamical model is proposed for describing the formation of superheavy nuclei in complete fusion reactions by incorporating the coupling of the relative motion to the nucleon transfer process. The capture of two heavy colliding nuclei, the formation of the compound nucleus and the de-excitation process are calculated by using an empirical coupled channel model, solving a master equation numerically and applying statistical theory, respectively. Evaporation residue excitation functions in cold fusion reactions are investigated systematically and compared with available experimental data. Maximal production cross sections of superheavy nuclei in cold fusion reactions with stable neutron-rich projectiles are obtained. Isotopic trends in the production of the superheavy elements Z=110, 112, 114, 116, 118 and 120 are analyzed systematically. Optimal combinations and the corresponding excitation energies are proposed.

  16. The Formation of the Wide Asynchronous Binary Asteroid Population

    E-Print Network [OSTI]

    Jacobson, Seth A; McMahon, Jay

    2013-01-01

    We propose and analyze a new mechanism for the formation of the wide asynchronous binary population. These binary asteroids have wide semi-major axes relative to most near-Earth and Main Belt asteroid systems. Confirmed members have rapidly rotating primaries and satellites that are not tidally locked. Previously suggested formation mechanisms from impact ejecta, planetary flybys and directly from rotational fission events cannot satisfy all of the observations. The newly hypothesized mechanism works as follows: (i) these systems are formed from rotational fission, (ii) their satellites are tidally locked, (iii) their orbits are expanded by the BYORP effect, (iv) their satellites de-synchronize due to the adiabatic invariance between the libration of the secondary and the mutual orbit, and (v) the secondary avoids resynchronization due to the the YORP effect. This seemingly complex chain of events is a natural pathway for binaries with satellites that have particular shapes, which define the BYORP effect torq...

  17. Bent-housing turbodrills improve hard-formation directional drilling

    SciTech Connect (OSTI)

    Koot, L.; Koole, K. (Shell U.K. Exploration and Production, Lowestoft (United Kingdom)); Gaynor, T. (Neyrfor-Weir Ltd., Aberdeen (United Kingdom))

    1993-02-15

    Improvements in the design of turbine-powered downhole motors allowed steerable drilling in a hard formation at a high rate of penetration (ROP). Drilling in this dolomite formation with the rotary or with positive-displacement motors (PDMs) was slow during steering operations. Shell's solution to the steering penetration rate problems was to change the well plans if suitable directional drilling tools weren't available. Where possible, the wells were designed with the Zechstein interval drilled as a tangent section with non-steerable turbodrills. However, a better solution was the use of a steerable turbodrill-a tool unavailable on the market at that time. The paper describes motor development, a field test, and the design and operation of the motor.

  18. THE FORMATION OF COSMIC FULLERENES FROM AROPHATIC CLUSTERS

    SciTech Connect (OSTI)

    Micelotta, Elisabetta R.; Cami, Jan; Peeters, Els; Fanchini, Giovanni; Jones, Anthony P.; Bernard-Salas, Jeronimo

    2012-12-10

    Fullerenes have recently been identified in space and they may play a significant role in the gas and dust budget of various astrophysical objects including planetary nebulae (PNe), reflection nebulae, and H II regions. The tenuous nature of the gas in these environments precludes the formation of fullerene materials following known vaporization or combustion synthesis routes even on astronomical timescales. We have studied the processing of hydrogenated amorphous carbon (a-C:H or HAC) nanoparticles and their specific derivative structures, which we name ''arophatics'', in the circumstellar environments of young, carbon-rich PNe. We find that UV-irradiation of such particles can result in the formation of fullerenes, consistent with the known physical conditions in PNe and with available timescales.

  19. Primordial magnetic fields and formation of molecular hydrogen

    E-Print Network [OSTI]

    Shiv K Sethi; Biman B. Nath; Kandaswamy Subramanian

    2008-04-22

    We study the implications of primordial magnetic fields for the thermal and ionization history of the post-recombination era. In particular we compute the effects of dissipation of primordial magnetic fields owing to ambipolar diffusion and decaying turbulence in the intergalactic medium (IGM) and the collapsing halos and compute the effects of the altered thermal and ionization history on the formation of molecular hydrogen. We show that, for magnetic field strengths in the range $2 \\times 10^{-10} {\\rm G} \\la B_0 \\la 2 \\times 10^{-9} {\\rm G}$, the molecular hydrogen fraction in IGM and collapsing halo can increase by a factor 5 to 1000 over the case with no magnetic fields. We discuss the implication of the increased molecular hydrogen fraction on the radiative transfer of UV photons and the formation of first structures in the universe.

  20. Soliton communication lines based on spectrally efficient modulation formats

    SciTech Connect (OSTI)

    Yushko, O V; Redyuk, A A

    2014-06-30

    We report the results of mathematical modelling of optical-signal propagation in soliton fibre-optic communication lines (FOCLs) based on spectrally efficient signal modulation formats. We have studied the influence of spontaneous emission noise, nonlinear distortions and FOCL length on the data transmission quality. We have compared the characteristics of a received optical signal for soliton and conventional dispersion compensating FOCLs. It is shown that in the presence of strong nonlinearity long-haul soliton FOCLs provide a higher data transmission performance, as well as allow higher order modulation formats to be used as compared to conventional communication lines. In the context of a coherent data transmission, soliton FOCLs allow the use of phase modulation with many levels, thereby increasing the spectral efficiency of the communication line. (optical communication lines)

  1. Ranging methods for developing wellbores in subsurface formations

    DOE Patents [OSTI]

    MacDonald, Duncan (Houston, TX)

    2011-09-06

    A method for forming two or more wellbores in a subsurface formation includes forming a first wellbore in the formation. A second wellbore is directionally drilled in a selected relationship relative to the first wellbore. At least one magnetic field is provided in the second wellbore using one or more magnets in the second wellbore located on a drilling string used to drill the second wellbore. At least one magnetic field is sensed in the first wellbore using at least two sensors in the first wellbore as the magnetic field passes by the at least two sensors while the second wellbore is being drilled. A position of the second wellbore is continuously assessed relative to the first wellbore using the sensed magnetic field. The direction of drilling of the second wellbore is adjusted so that the second wellbore remains in the selected relationship relative to the first wellbore.

  2. Elliptical Galaxy Dynamics: The Issues Pertaining to Galaxy Formation

    E-Print Network [OSTI]

    David Burstein

    1999-08-31

    How elliptical galaxy dynamics relate to galaxy structure, stellar populations, spiral galaxies and environment are reviewed. The evidence assembled shows that most, if not all, galaxies originally classified as gE contain disks within them. Taken together, the existing evidence are most consistent with the gravitational, hierarchical, clustering, merging (HCM) concept that all galaxies, including gE, are formed from the combination of much smaller galaxies. Within the HCM picture, the evidence also strongly suggests that the subunits which go into forming galaxies must be related in specific ways both to the mass of the galaxy they will form, and to the environment in which the galaxy forms. Despite the extensive data that we now have on galaxies that can constrain their formation history, the lack of a physical understanding of the stellar initial mass function prevents us from developing realistic physical models for galaxy formation.

  3. Studying Structure Formation With Large Galaxy Redshift Surveys

    E-Print Network [OSTI]

    David H. Weinberg

    1994-09-30

    I outline the connections between some of the most widely used statistical measures of galaxy clustering and the fundamental issues in the theory of structure formation. I devote particular attention to the problem of biasing, i.e. to a possible difference between the distribution of galaxies and the distribution of mass. Using numerical experiments, I show that a local morphology-density relation leads to different slopes and amplitudes for the correlation functions of different galaxy types on small scales, but that the correlation functions on large scales all have the same shape, differing only by constant factors. I also examine a variety of biasing models in which the efficiency of galaxy formation depends on local properties of the mass distribution. While these purely local influences do lead to a large-scale bias, in all cases the bias factor becomes constant on scales larger than the galaxy correlation length.

  4. Reservoir characterization of the Smackover Formation in southwest Alabama

    SciTech Connect (OSTI)

    Kopaska-Merkel, D.C.; Hall, D.R.; Mann, S.D.; Tew, B.H.

    1993-02-01

    The Upper Jurassic Smackover Formation is found in an arcuate belt in the subsurface from south Texas to panhandle Florida. The Smackover is the most prolific hydrocarbon-producing formation in Alabama and is an important hydrocarbon reservoir from Florida to Texas. In this report Smackover hydrocarbon reservoirs in southwest Alabama are described. Also, the nine enhanced- and improved-recovery projects that have been undertaken in the Smackover of Alabama are evaluated. The report concludes with recommendations about potential future enhanced- and improved-recovery projects in Smackover reservoirs in Alabama and an estimate of the potential volume of liquid hydrocarbons recoverable by enhanced- and improved-recovery methods from the Smackover of Alabama.

  5. Crystal Structure Representations for Machine Learning Models of Formation Energies

    E-Print Network [OSTI]

    Faber, Felix; von Lilienfeld, O Anatole; Armiento, Rickard

    2015-01-01

    We introduce and evaluate a set of feature vector representations of crystal structures for machine learning (ML) models of formation energies of solids. ML models of atomization energies of organic molecules have been successful using a Coulomb matrix representation of the molecule. We consider three ways to generalize such representations to periodic systems: (i) a matrix where each element is related to the Ewald sum of the electrostatic interaction between two different atoms in the unit cell repeated over the lattice; (ii) an extended Coulomb-like matrix that takes into account a number of neighboring unit cells; and (iii) an Ansatz that mimics the periodicity and the basic features of the elements in the Ewald sum matrix by using a sine function of the crystal coordinates of the atoms. The representations are compared for a Laplacian kernel with Manhattan norm, trained to reproduce formation energies using a data set of 3938 crystal structures obtained from the Materials Project. For training sets consi...

  6. A Look At Three Different Scenarios for Bulge Formation

    E-Print Network [OSTI]

    Rychard J. Bouwens; Laura Cayon; Joseph Silk

    1998-12-10

    In this paper, we present three qualitatively different scenarios for bulge formation: a secular evolution model in which bulges form after disks and undergo several central starbursts, a primordial collapse model in which bulges and disks form simultaneously, and an early bulge formation model in which bulges form prior to disks. We normalize our models to the local z=0 observations of de Jong & van der Kruit (1994) and Peletier & Balcells (1996) and make comparisons with high redshift observations. We consider model predictions relating directly to bulge-to-disk properties. As expected, smaller bulge-to-disk ratios and bluer bulge colors are predicted by the secular evolution model at all redshifts, although uncertainties in the data are currently too large to differentiate strongly between the models.

  7. SAR image formation with azimuth interpolation after azimuth transform

    DOE Patents [OSTI]

    Doerry; Armin W. (Albuquerque, NM), Martin; Grant D. (Marlborough, MA), Holzrichter; Michael W. (Albuquerque, NM)

    2008-07-08

    Two-dimensional SAR data can be processed into a rectangular grid format by subjecting the SAR data to a Fourier transform operation, and thereafter to a corresponding interpolation operation. Because the interpolation operation follows the Fourier transform operation, the interpolation operation can be simplified, and the effect of interpolation errors can be diminished. This provides for the possibility of both reducing the re-grid processing time, and improving the image quality.

  8. Diagenesis within the deep Tuscaloosa formation, Profit Island field, Louisiana 

    E-Print Network [OSTI]

    Hudder, Karen Ann Gilchrist

    1982-01-01

    The lower Tuscaloosa Formation of south-central Louisiana is a prolific and highly potential deep gas reservoir. Of particular interest are the unusually high porosity and permeability values for the age, depth, and temperature of the rocks. In the Profit... hydrocarbon accumulation and production in reservoirs, particularly from such unusually porous and permeable rocks. THE TUSCALOOSA TREND Regional Setting The deep Tuscaloosa trend encompasses an area of south-central Louisiana measuring approximately 200...

  9. Method for recovering oil from an underground formation

    SciTech Connect (OSTI)

    Hesselink, F.T.; Saidi, A.M.

    1982-12-21

    Method for recovering oil from an underground formation consisting of blocks of relatively low permeability with an oilwet pore space containing oil surrounded by a fracture network of relatively high permeability by supplying to the fracture network an aqueous solution of a surfactant adapted for decreasing the surface tension between water and oil and displacing the oil from the oil-wet pore space of the blocks.

  10. FILAMENTARY STAR FORMATION: OBSERVING THE EVOLUTION TOWARD FLATTENED ENVELOPES

    SciTech Connect (OSTI)

    Lee, Katherine; Looney, Leslie; Johnstone, Doug; Tobin, John E-mail: lwl@illinois.edu E-mail: jtobin@nrao.edu

    2012-12-20

    Filamentary structures are ubiquitous from large-scale molecular clouds (a few parsecs) to small-scale circumstellar envelopes around Class 0 sources ({approx}1000 AU to {approx}0.1 pc). In particular, recent observations with the Herschel Space Observatory emphasize the importance of large-scale filaments (a few parsecs) and star formation. The small-scale flattened envelopes around Class 0 sources are reminiscent of the large-scale filaments. We propose an observationally derived scenario for filamentary star formation that describes the evolution of filaments as part of the process for formation of cores and circumstellar envelopes. If such a scenario is correct, small-scale filamentary structures (0.1 pc in length) with higher densities embedded in starless cores should exist, although to date almost all the interferometers have failed to observe such structures. We perform synthetic observations of filaments at the prestellar stage by modeling the known Class 0 flattened envelope in L1157 using both the Combined Array for Research in Millimeter-wave Astronomy (CARMA) and the Atacama Large Millimeter/Submillimeter Array (ALMA). We show that with reasonable estimates for the column density through the flattened envelope, the CARMA D array at 3 mm wavelengths is not able to detect such filamentary structure, so previous studies would not have detected them. However, the substructures may be detected with the CARMA D+E array at 3 mm and the CARMA E array at 1 mm as a result of more appropriate resolution and sensitivity. ALMA is also capable of detecting the substructures and showing the structures in detail compared to the CARMA results with its unprecedented sensitivity. Such detection will confirm the new proposed paradigm of non-spherical star formation.

  11. Water confined in nanopores: spontaneous formation of microcavities

    E-Print Network [OSTI]

    John Russo; Simone Melchionna; Francesco De Luca; Cinzia Casieri

    2007-05-16

    Molecular Dynamics simulations of water confined in nanometer sized, hydrophobic channels show that water forms localized cavities for pore diameter ~ 2.0 nm. The cavities present non-spherical shape and lay preferentially adjacent to the confining wall inducing a peculiar form to the liquid exposed surface. The regime of localized cavitation appears to be correlated with the formation of a vapor layer, as predicted by the Lum-Chandler-Weeks theory, implying partial filling of the pore.

  12. Galaxy formation & evolution: the far-ir/sub-mm view

    E-Print Network [OSTI]

    M. Cirasuolo; J. S. Dunlop

    2008-10-07

    We review our current knowledge of the population of high-redshift sub-mm/mm galaxies, with particular emphasis on recent results from the SCUBA HAlf Degree Extragalactic Survey (SHADES). All available evidence indicates that these objects form the high-redshift, high-luminosity, high-mass tail of the dusty starforming galaxy population revealed at lower redshifts and luminosities by Spitzer. Current theoretical models of galaxy formation struggle to reproduce these extreme objects in the numbers indicated by current surveys.

  13. Solar System Processes Underlying Planetary Formation, Geodynamics, and the Georeactor

    E-Print Network [OSTI]

    J. Marvin Herndon

    2007-01-02

    Only three processes, operant during the formation of the Solar System, are responsible for the diversity of matter in the Solar System and are directly responsible for planetary internal-structures, including planetocentric nuclear fission reactors, and for dynamical processes, including and especially, geodynamics. These processes are: (i) Low-pressure, low-temperature condensation from solar matter in the remote reaches of the Solar System or in the interstellar medium; (ii) High-pressure, high-temperature condensation from solar matter associated with planetary-formation by raining out from the interiors of giant-gaseous protoplanets, and; (iii) Stripping of the primordial volatile components from the inner portion of the Solar System by super-intense solar wind associated with T-Tauri phase mass-ejections, presumably during the thermonuclear ignition of the Sun. As described herein, these processes lead logically, in a causally related manner, to a coherent vision of planetary formation with profound implications including, but not limited to, (a) Earth formation as a giant gaseous Jupiter-like planet with vast amounts of stored energy of protoplanetary compression in its rock-plus-alloy kernel; (b) Removal of approximately 300 Earth-masses of primordial gases from the Earth, which began Earth's decompression process, making available the stored energy of protoplanetary compression for driving geodynamic processes, which I have described by the new whole-Earth decompression dynamics and which is responsible for emplacing heat at the mantle-crust-interface at the base of the crust through the process I have described, called mantle decompression thermal-tsunami; and, (c)Uranium accumulations at the planetary centers capable of self-sustained nuclear fission chain reactions.

  14. Downhole burner systems and methods for heating subsurface formations

    DOE Patents [OSTI]

    Farmayan, Walter Farman (Houston, TX); Giles, Steven Paul (Damon, TX); Brignac, Jr., Joseph Phillip (Katy, TX); Munshi, Abdul Wahid (Houston, TX); Abbasi, Faraz (Sugarland, TX); Clomburg, Lloyd Anthony (Houston, TX); Anderson, Karl Gregory (Missouri City, TX); Tsai, Kuochen (Katy, TX); Siddoway, Mark Alan (Katy, TX)

    2011-05-31

    A gas burner assembly for heating a subsurface formation includes an oxidant conduit, a fuel conduit, and a plurality of oxidizers coupled to the oxidant conduit. At least one of the oxidizers includes a mix chamber for mixing fuel from the fuel conduit with oxidant from the oxidant conduit, an igniter, and a shield. The shield includes a plurality of openings in communication with the oxidant conduit. At least one flame stabilizer is coupled to the shield.

  15. Planning Formative Assessment Workshop 2012 J.A.Nychka

    E-Print Network [OSTI]

    MacMillan, Andrew

    ching Go nd Cross TGI p ents/Teachin tgi/data_entr or course _ tive Asse als Inven please do so a g? o assess? e the holistic a tion, activitie erta.ca/docume tive Asse ded Learn nt clearly und and Community nkClick.aspx?file g Format y College: eticket=%2F0BA4 tive Asse 4qlDaAE%3D&ta essment abid=3938

  16. Room-temperature Formation of Hollow Cu2O Nanoparticles

    SciTech Connect (OSTI)

    Hung, Ling-I; Tsung, Chia-Kuang; Huang, Wenyu; Yang, Peidong

    2010-01-18

    Monodisperse Cu and Cu2O nanoparticles (NPs) are synthesized using tetradecylphosphonic acid as a capping agent. Dispersing the NPs in chloroform and hexane at room temperature results in the formation of hollow Cu2O NPs and Cu@Cu2O core/shell NPs, respectively. The monodisperse Cu2O NPs are used to fabricate hybrid solar cells with efficiency of 0.14percent under AM 1.5 and 1 Sun illumination.

  17. Measurement of the Formation Rate of Muonic Hydrogen Molecules

    E-Print Network [OSTI]

    MuCap Collaboration; V. A. Andreev; T. I. Banks; R. M. Carey; T. A. Case; S. M. Clayton; K. M. Crowe; J. Deutsch; J. Egger; S. J. Freedman; V. A. Ganzha; T. Gorringe; F. E. Gray; D. W. Hertzog; M. Hildebrandt; P. Kammel; B. Kiburg; S. Knaack; P. A. Kravtsov; A. G. Krivshich; B. Lauss; K. R. Lynch; E. M. Maev; O. E. Maev; F. Mulhauser; C. Petitjean; G. E. Petrov; R. Prieels; G. N. Schapkin; G. G. Semenchuk; M. A. Soroka; V. Tishchenko; A. A. Vasilyev; A. A. Vorobyov; M. E. Vznuzdaev; P. Winter

    2015-02-03

    Background: The rate \\lambda_pp\\mu\\ characterizes the formation of pp\\mu\\ molecules in collisions of muonic p\\mu\\ atoms with hydrogen. In measurements of the basic weak muon capture reaction on the proton to determine the pseudoscalar coupling g_P, capture occurs from both atomic and molecular states. Thus knowledge of \\lambda_pp\\mu\\ is required for a correct interpretation of these experiments. Purpose: Recently the MuCap experiment has measured the capture rate \\Lambda_S from the singlet p\\mu\\ atom, employing a low density active target to suppress pp\\mu\\ formation (PRL 110, 12504 (2013)). Nevertheless, given the unprecedented precision of this experiment, the existing experimental knowledge in \\lambda_pp\\mu\\ had to be improved. Method: The MuCap experiment derived the weak capture rate from the muon disappearance rate in ultra-pure hydrogen. By doping the hydrogen with 20 ppm of argon, a competing process to pp\\mu\\ formation was introduced, which allowed the extraction of \\lambda_pp\\mu\\ from the observed time distribution of decay electrons. Results: The pp\\mu\\ formation rate was measured as \\lambda_pp\\mu = (2.01 +- 0.06(stat) +- 0.03(sys)) 10^6 s^-1. This result updates the \\lambda_pp\\mu\\ value used in the above mentioned MuCap publication. Conclusions: The 2.5x higher precision compared to earlier experiments and the fact that the measurement was performed at nearly identical conditions to the main data taking, reduces the uncertainty induced by \\lambda_pp\\mu\\ to a minor contribution to the overall uncertainty of \\Lambda_S and g_P, as determined in MuCap. Our final value for \\lambda_pp\\mu\\ shifts \\Lambda_S and g_P by less than one tenth of their respective uncertainties compared to our results published earlier.

  18. Practical Issues in Formation Control of Multi-Robot Systems 

    E-Print Network [OSTI]

    Zhang, Junjie

    2010-07-14

    of Multi-Robot Systems. (May 2010) Junjie Zhang, B.S., Dalian University of Technology; M.S., University of Michigan-Ann Arbor Chair of Advisory Committee: Dr. Suhada Jayasuriya Considered in this research is a framework for effective formation control... to include housework assistance, patient rehabilitation, industrial automation, automated highways, geophysical mapping, facility monitoring and detection, disaster relief, and space exploration. In all the aforementioned applications, multiple robots...

  19. Ionized gas kinematics and massive star formation in NGC 1530

    E-Print Network [OSTI]

    A. Zurita; M. Relano; J. E. Beckman; J. H. Knapen

    2003-07-11

    We present emission line mapping of the strongly barred galaxy NGC 1530 obtained from Fabry-Perot interferometry in Halpha, at significantly enhanced angular resolution compared with published studies. The main point of the work is to examine in detail the non-circular components of the velocity field of the gas, presumably induced by the strongly non-axisymmetric gravitational potential of the bar. These reveal quasi-elliptical motions with speeds of order 100 km/s aligned with the bar. It also shows how these flows swing in towards and around the nucleus as they cross a circumnuclear resonance, from the dominant "x1 orbits" outside the resonance to "x2 orbits" within it. Comparing cross-sections of the residual velocity map along and across the bar with the Halpha intensity map indicates a systematic offset between regions of high non-circular velocity and massive star formation. To investigate further we produce velocity gradient maps along and across the bar. These illustrate very nicely the shear compression of the gas, revealed by the location of the dust lanes along loci of maximum velocity gradient perpendicular to the bar. They also show clearly how shear acts to inhibit massive star formation, whereas shocks act to enhance it. Although the inhibiting effect of gas shear flow on star formation has long been predicted, this is the clearest observational illustration so far of the effect. It is also the clearest evidence that dust picks out shock-induced inflow along bars. These observations should be of considerable interest to those modelling massive star formation in general.

  20. Numerical studies of galaxy formation using special purpose hardware

    E-Print Network [OSTI]

    Matthias Steinmetz

    2002-01-25

    I review recent progress in numerically simulating the formation and evolution of galaxies in hierarchically clustering universes. Special emphasis is given to results based on high-resolution gas dynamical simulations using the N-body hardware integrator GRAPE. Applications address the origin of the spin of disk galaxies, the structure and kinematics of damped Lyman-alpha systems, and the origin of galaxy morphology and of galaxy scaling laws.

  1. Effect of Poisson ratio on cellular structure formation

    E-Print Network [OSTI]

    Ilka B. Bischofs; Ulrich S. Schwarz

    2005-04-05

    Mechanically active cells in soft media act as force dipoles. The resulting elastic interactions are long-ranged and favor the formation of strings. We show analytically that due to screening, the effective interaction between strings decays exponentially, with a decay length determined only by geometry. Both for disordered and ordered arrangements of cells, we predict novel phase transitions from paraelastic to ferroelastic and anti-ferroelastic phases as a function of Poisson ratio.

  2. ARTIFACT FORMATION DURING NEUTRALIZATION OF TANK 50 SAMPLES

    SciTech Connect (OSTI)

    Crump, S.; Young, J.

    2014-08-01

    Degradation products have been identified in the extracts of Tank 50 samples analyzed by semivolatile organic compound analysis (SVOA) using gas chromatography/mass spectrometry (GC/MS). These materials, identified as short chain alkyl alcohols, were formed by acidification during sample preparation. A number of questions were raised about the formation of these and other materials reported in Tank 50 surface samples, and this report serves to address these questions.

  3. Method and apparatus for production of subsea hydrocarbon formations

    SciTech Connect (OSTI)

    Blandford, Joseph W.

    1992-01-01

    A well tender system for controlling, separating, storing and offloading well fluids produced from subsea hydrocarbon formations. The system comprises a vertically aligned series of tethered cylindrical tanks which are torsionally stabilized by flexible catenary production riser and expert riser bundles, and serviced by separate catenary pipe bundles. Piles are secured to the seabed, each pile assembly being pivotally connected to a lower rigid tendon, which is in turn connected to tendons arranged about the periphery of the interconnected cylindrical tanks.

  4. Method and apparatus for production of subsea hydrocarbon formations

    DOE Patents [OSTI]

    Blandford, Joseph W. (15 Mott La., Houston, TX 77024)

    1994-01-01

    A well tender system for controlling, separating, storing and offloading well fluids produced from subsea hydrocarbon formations. The system comprises a vertically aligned series of tethered cylindrical tanks which are torsionally stabilized by flexible catenary production riser and export riser bundles, and serviced by separate catenary pipe bundles. Piles are secured to the seabed, each pile assembly being pivotally connected to a lower rigid tendon, which is in turn connected to tendons arranged about the periphery of the interconnected cylindrical tanks.

  5. Data from selected Almond Formation outcrops -- Sweetwater County, Wyoming

    SciTech Connect (OSTI)

    Jackson, S.R.; Rawn-Schatzinger, V.

    1993-12-01

    The objectives of this research program are to: (1) determine the reservoir characteristics and production problems of shoreline barrier reservoirs; and (2) develop methods and methodologies to effectively characterize shoreline barrier reservoirs to predict flow patterns of injected and produced fluids. Two reservoirs were selected for detailed reservoir characterization studies -- Bell Creek field, Carter County, Montana, that produces from the Lower Cretaceous (Albian-Cenomanian) Muddy Formation, and Patrick Draw field, Sweetwater County, Wyoming that produces from the Upper Cretaceous (Campanian) Almond Formation of the Mesaverde Group. An important component of the research project was to use information from outcrop exposures of the producing formations to study the spatial variations of reservoir properties and the degree to which outcrop information can be used in the construction of reservoir models. A report similar to this one presents the Muddy Formation outcrop data and analyses performed in the course of this study (Rawn-Schatzinger, 1993). Two outcrop localities, RG and RH, previously described by Roehler (1988) provided good exposures of the Upper Almond shoreline barrier facies and were studied during 1990--1991. Core from core well No. 2 drilled approximately 0.3 miles downdip of outcrop RG was obtained for study. The results of the core study will be reported in a separate volume. Outcrops RH and RG, located about 2 miles apart were selected for detailed description and drilling of core plugs. One 257-ft-thick section was measured at outcrop RG, and three sections {approximately}145 ft thick located 490 and 655 feet apart were measured at the outcrop RH. Cross-sections of these described profiles were constructed to determine lateral facies continuity and changes. This report contains the data and analyses from the studied outcrops.

  6. In situ recovery from residually heated sections in a hydrocarbon containing formation

    DOE Patents [OSTI]

    Vinegar, Harold J. (Bellaire, TX); Karanikas, John Michael (Houston, TX); Ryan, Robert Charles (Houston, TX)

    2010-12-14

    Methods of treating a tar sands formation is described herein. The methods may include providing heat to a first section of a hydrocarbon layer in the formation from a plurality of heaters located in the first section of the formation. Heat is transferred from the heaters so that at least a first section of the formation reaches a selected temperature. At least a portion of residual heat from the first section transfers from the first section to a second section of the formation. At least a portion of hydrocarbons in the second section are mobilized by providing a solvation fluid and/or a pressurizing fluid to the second section of the formation.

  7. EXPLOITATION AND OPTIMIZATION OF RESERVOIR PERFORMANCE IN HUNTON FORMATION, OKLAHOMA

    SciTech Connect (OSTI)

    Mohan Kelkar

    2003-04-01

    West Carney Field produces from Hunton Formation. All the wells produce oil, water and gas. The main objective of this study is to understand the unique behavior observed in the field. This behavior includes: (1) Decrease in WOR over time; (2) Decrease in GOR at initial stages; (3) High decline rates of oil and gas; and (4) strong hydrodynamic connectivity between wells. This report specifically addresses two issues relevant to our understanding of the West Carney reservoir. By using core and log data as well as fluorescence information, we demonstrate that our hypothesis of how the reservoir is formed is consistent with these observations. Namely, oil migrated in water wet reservoir, over time, oil changed the wettability of some part of the reservoir, oil eventually leaked to upper formations prompting re-introduction of water into reservoir. Because of change in wettability, different pore size distributions responded differently to water influx. This hypothesis is consistent with fluorescence and porosity data, as we explain it in this quarterly report. The second issue deals with how to best calculate connected oil volume in the reservoir. The log data does not necessarily provide us with relevant information regarding oil in place. However, we have developed a new material balance technique to calculate the connected oil volume based on observed pressure and production data. By using the technique to four different fields producing from Hunton formation, we demonstrate that the technique can be successfully applied to calculate the connected oil in place.

  8. EXPLOITATION AND OPTIMIZATION OF RESERVOIR PERFORMANCE IN HUNTON FORMATION, OKLAHOMA

    SciTech Connect (OSTI)

    Mohan Kelkar

    2005-02-01

    Hunton formation in Oklahoma has displayed some unique production characteristics. These include high initial water-oil and gas-oil ratios, decline in those ratios over time and temporary increase in gas-oil ratio during pressure build up. The formation also displays highly complex geology, but surprising hydrodynamic continuity. This report addresses three key issues related specifically to West Carney Hunton field and, in general, to any other Hunton formation exhibiting similar behavior: (1) What is the primary mechanism by which oil and gas is produced from the field? (2) How can the knowledge gained from studying the existing fields can be extended to other fields which have the potential to produce? (3) What can be done to improve the performance of this reservoir? We have developed a comprehensive model to explain the behavior of the reservoir. By using available production, geological, core and log data, we are able to develop a reservoir model which explains the production behavior in the reservoir. Using easily available information, such as log data, we have established the parameters needed for a field to be economically successful. We provide guidelines in terms of what to look for in a new field and how to develop it. Finally, through laboratory experiments, we show that surfactants can be used to improve the hydrocarbons recovery from the field. In addition, injection of CO{sub 2} or natural gas also will help us recover additional oil from the field.

  9. FORMATION OF CIRCUMBINARY PLANETS IN A DEAD ZONE

    SciTech Connect (OSTI)

    Martin, Rebecca G.; Armitage, Philip J. [JILA, University of Colorado and NIST, UCB 440, Boulder, CO 80309 (United States); Alexander, Richard D. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom)

    2013-08-10

    Circumbinary planets have been observed at orbital radii where binary perturbations may have significant effects on the gas disk structure, on planetesimal velocity dispersion, and on the coupling between turbulence and planetesimals. Here, we note that the impact of all of these effects on planet formation is qualitatively altered if the circumbinary disk structure is layered, with a non-turbulent midplane layer (dead zone) and strongly turbulent surface layers. For close binaries, we find that the dead zone typically extends from a radius close to the inner disk edge up to a radius of around 10-20 AU from the center of mass of the binary. The peak in the surface density occurs within the dead zone, far from the inner disk edge, close to the snow line, and may act as a trap for aerodynamically coupled solids. We suggest that circumbinary planet formation may be easier near this preferential location than for disks around single stars. However, dead zones around wide binaries are less likely, and hence planet formation may be more difficult there.

  10. Mineral ecophysiological evidence for microbial activity in banded iron formation

    SciTech Connect (OSTI)

    Li, Dr. Yi-Liang [University of Tennessee, Knoxville (UTK); Konhauser, Dr, Kurt [University of Alberta; Cole, David R [ORNL; Phelps, Tommy Joe [ORNL

    2011-01-01

    The phosphorus composition of banded-iron formations (BIFs) has been used as a proxy for Precambrian seawater composition and the paleoeredox state of Earth's surface environment. However, it is unclear whether the phosphorus in BIFs originally entered the sediment as a sorbed component of the iron oxyhydroxide particles, or whether it was incorporated into the biomass of marine phytoplankton. We conducted high-resolution mineral analyses and report here the first detection of an Fe(III) acetate salt, as well as nanocrystals of apatite in association with magnetite, in the 2.48 Ga Dales Gorge Member of the Brockman Iron Formation (a BIF), Hamersley, Western Australia. The clusters of apatite are similar in size and morphology to biogenic apatite crystals resulting from biomass decay in Phanerozoic marine sediments, while the formation of an Fe(III) acetate salt and magnetite not only implies the original presence of biomass in the BIF sediments, but also that organic carbon likely served as an electron donor during bacterial Fe(III) reduction. This study is important because it suggests that phytoplankton may have played a key role in the transfer of phosphorus (and other trace elements) from the photic zone to the seafloor.

  11. Measurement of the Formation Rate of Muonic Hydrogen Molecules

    E-Print Network [OSTI]

    Andreev, V A; Carey, R M; Case, T A; Clayton, S M; Crowe, K M; Deutsch, J; Egger, J; Freedman, S J; Ganzha, V A; Gorringe, T; Gray, F E; Hertzog, D W; Hildebrandt, M; Kammel, P; Kiburg, B; Knaack, S; Kravtsov, P A; Krivshich, A G; Lauss, B; Lynch, K R; Maev, E M; Maev, O E; Mulhauser, F; Petitjean, C; Petrov, G E; Prieels, R; Schapkin, G N; Semenchuk, G G; Soroka, M A; Tishchenko, V; Vasilyev, A A; Vorobyov, A A; Vznuzdaev, M E; Winter, P

    2015-01-01

    Background: The rate \\lambda_pp\\mu\\ characterizes the formation of pp\\mu\\ molecules in collisions of muonic p\\mu\\ atoms with hydrogen. In measurements of the basic weak muon capture reaction on the proton to determine the pseudoscalar coupling g_P, capture occurs from both atomic and molecular states. Thus knowledge of \\lambda_pp\\mu\\ is required for a correct interpretation of these experiments. Purpose: Recently the MuCap experiment has measured the capture rate \\Lambda_S from the singlet p\\mu\\ atom, employing a low density active target to suppress pp\\mu\\ formation (PRL 110, 12504 (2013)). Nevertheless, given the unprecedented precision of this experiment, the existing experimental knowledge in \\lambda_pp\\mu\\ had to be improved. Method: The MuCap experiment derived the weak capture rate from the muon disappearance rate in ultra-pure hydrogen. By doping the hydrogen with 20 ppm of argon, a competing process to pp\\mu\\ formation was introduced, which allowed the extraction of \\lambda_pp\\mu\\ from the observed t...

  12. SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION

    SciTech Connect (OSTI)

    Cheung, M. C. M.; Title, A. M. [Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304 (United States); Rempel, M. [High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307 (United States); Schuessler, M. [Max Planck Institute for Solar System Research, Katlenburg-Lindau, 37191 (Germany)

    2010-09-01

    We present a radiative magnetohydrodynamics simulation of the formation of an active region (AR) on the solar surface. The simulation models the rise of a buoyant magnetic flux bundle from a depth of 7.5 Mm in the convection zone up into the solar photosphere. The rise of the magnetic plasma in the convection zone is accompanied by predominantly horizontal expansion. Such an expansion leads to a scaling relation between the plasma density and the magnetic field strength such that B {proportional_to} rhov{sup 1/2}. The emergence of magnetic flux into the photosphere appears as a complex magnetic pattern, which results from the interaction of the rising magnetic field with the turbulent convective flows. Small-scale magnetic elements at the surface first appear, followed by their gradual coalescence into larger magnetic concentrations, which eventually results in the formation of a pair of opposite polarity spots. Although the mean flow pattern in the vicinity of the developing spots is directed radially outward, correlations between the magnetic field and velocity field fluctuations allow the spots to accumulate flux. Such correlations result from the Lorentz-force-driven, counterstreaming motion of opposite polarity fragments. The formation of the simulated AR is accompanied by transient light bridges between umbrae and umbral dots. Together with recent sunspot modeling, this work highlights the common magnetoconvective origin of umbral dots, light bridges, and penumbral filaments.

  13. NO[sub x] formation in unsteady combustion

    SciTech Connect (OSTI)

    Norton, T.S.; Richards, G.A. (USDOE Morgantown Energy Technology Center, WV (United States)); Narayanaswami, L.L. (Embry-Riddle Aeronautical Univ., Daytona Beach, FL (United States))

    1992-01-01

    It has been found that fuel-lean operating conditions produce the best results for the current aerovalve pulse combustor. Under these conditions, the levels of unburned hydrocarbon pollutants in the exhaust stream are negligibly low. Initial results on CO indicate that the gas chromatograph method (thermal conductivity detector) is not sensitive enough to measure concentrations below 500 ppM. The modeling work involves the modification of an existing Thermal Pulse Combustor code to include some detailed chemistry. Two methods are used. In the first method, a kinetic mechanism for the formation of thermal NO is superimposed onto the oscillating field of temperature and pressure predicted by the existing pulse combustor model. The concentrations of oxygen atoms and N[sub 2], which control the NO formation step, are estimated from an equilibrium calculation at each temperature and pressure condition. Then the NO formation rate is determined from the rate of the reaction N[sub 2] + 0 --> NO + N. In the second method, more detailed chemistry is incorporated into the base model and the chemical heat release equations are used to drive the pulsations instead of vice versa. The 0-atom concentration is determined from a complex series of chain reactions, rather than by equilibrium.

  14. NO{sub x} formation in unsteady combustion

    SciTech Connect (OSTI)

    Norton, T.S.; Richards, G.A. [USDOE Morgantown Energy Technology Center, WV (United States); Narayanaswami, L.L. [Embry-Riddle Aeronautical Univ., Daytona Beach, FL (United States)

    1992-12-01

    It has been found that fuel-lean operating conditions produce the best results for the current aerovalve pulse combustor. Under these conditions, the levels of unburned hydrocarbon pollutants in the exhaust stream are negligibly low. Initial results on CO indicate that the gas chromatograph method (thermal conductivity detector) is not sensitive enough to measure concentrations below 500 ppM. The modeling work involves the modification of an existing Thermal Pulse Combustor code to include some detailed chemistry. Two methods are used. In the first method, a kinetic mechanism for the formation of thermal NO is superimposed onto the oscillating field of temperature and pressure predicted by the existing pulse combustor model. The concentrations of oxygen atoms and N{sub 2}, which control the NO formation step, are estimated from an equilibrium calculation at each temperature and pressure condition. Then the NO formation rate is determined from the rate of the reaction N{sub 2} + 0 --> NO + N. In the second method, more detailed chemistry is incorporated into the base model and the chemical heat release equations are used to drive the pulsations instead of vice versa. The 0-atom concentration is determined from a complex series of chain reactions, rather than by equilibrium.

  15. Solvent-quality dependent contact formation dynamics in proteins

    E-Print Network [OSTI]

    Kundu, Prasanta

    2015-01-01

    The mean time of contact formation between two ends of a protein chain shows power law dependence with respect to the number of residues, $\\tau_{CF} \\sim N^{\\alpha}$. Fluorescence quenching measurements based on triplet-triplet energy transfer show variation in the value of scaling exponent $\\alpha$ for different protein-solvent systems. Here, starting from a non-Markovian diffusion equation supplemented with an exponential sink term that accounts for the energy transfer reaction between donor and acceptor groups, we calculate the mean time of contact formation using the Wilemski-Fixman closure approximation. The non-Markovian diffusion-reaction equation includes the effects of solvent quality and hydrodynamic interaction in a mean-field fashion. It shows that the contact formation dynamics is mainly governed by two time scales, the reciprocal of the intrinsic rate of quenching $(k_0^{ET})^{-1}$, and the relaxation time $\\tau_0 = \\eta b^3/k_B T$ of the coarse-grained residue of an effective size $b$ with solv...

  16. Coulomb effects on the formation of proton halo nuclei

    E-Print Network [OSTI]

    Yu-Jie Liang; Yan-Song Li; Fu-Guo Deng; Xi-Han Li; Bao-An Bian; Feng-Shou Zhang; Zu-Hua Liu; Hong-Yu Zhou

    2007-08-01

    The exotic structures in the 2s_{1/2} states of five pairs of mirror nuclei ^{17}O-^{17}F, ^{26}Na-^{26}P, ^{27}Mg-^{27}P, ^{28}Al-^{28}P and ^{29}Si-^{29}P are investigated with the relativistic mean-field (RMF) theory and the single-particle model (SPM) to explore the role of the Coulomb effects on the proton halo formation. The present RMF calculations show that the exotic structure of the valence proton is more obvious than that of the valence neutron of its mirror nucleus, the difference of exotic size between each mirror nuclei becomes smaller with the increase of mass number A of the mirror nuclei and the ratios of the valence proton and valence neutron root-mean-square (RMS) radius to the matter radius in each pair of mirror nuclei all decrease linearly with the increase of A. In order to interpret these results, we analyze two opposite effects of Coulomb interaction on the exotic structure formation with SPM and find that the contribution of the energy level shift is more important than that of the Coulomb barrier for light nuclei. However, the hindrance of the Coulomb barrier becomes more obvious with the increase of A. When A is larger than 34, Coulomb effects on the exotic structure formation will almost become zero because its two effects counteract with each other.

  17. Environmental regulation of cloud and star formation in galactic bars

    E-Print Network [OSTI]

    Renaud, F; Emsellem, E; Agertz, O; Athanassoula, E; Combes, F; Elmegreen, B; Kraljic, K; Motte, F; Teyssier, R

    2015-01-01

    The strong time-dependence of the dynamics of galactic bars yields a complex and rapidly evolving distribution of dense gas and star forming regions. Although bars mainly host regions void of any star formation activity, their extremities can gather the physical conditions for the formation of molecular complexes and mini-starbursts. Using a sub-parsec resolution hydrodynamical simulation of a Milky Way-like galaxy, we probe these conditions to explore how and where bar (hydro-)dynamics favours the formation or destruction of molecular clouds and stars. The interplay between the kpc-scale dynamics (gas flows, shear) and the parsec-scale (turbulence) is key to this problem. We find a strong dichotomy between the leading and trailing sides of the bar, in term of cloud fragmentation and in the age distribution of the young stars. After orbiting along the bar edge, these young structures slow down at the extremities of the bar, where orbital crowding increases the probability of cloud-cloud collision. We find tha...

  18. The Role of Heating and Enrichment in Galaxy Formation

    E-Print Network [OSTI]

    Evan Scannapieco; Tom Broadhurst

    2000-10-11

    We show that the winds identified with high-redshift low-mass galaxies may strongly affect the formation of stars in more massive galaxies that form later. With 3D realizations of a simple linear growth model we track gas shocking, metal enrichment, and cooling, together with dark halo formation. We show that outflows typically strip baryonic material out of collapsing intermediate mass halos, suppressing star formation. More massive halos can trap the heated gas but collapse late, leading to a broad bimodal redshift distribution, with a larger characteristic mass associated with the lower redshift peak. This scenario accounts for the observed bell-shaped luminosity function of early type galaxies, explains the small number of Milky Way satellite galaxies relative to Cold Dark Matter models predictions, and provides a possible explanation for the lack of metal poor G-dwarfs in the solar neighborhood and the more general lack of low-metallicity stars in massive galaxies relative to ``closed-box'' models of chemical enrichment. Intergalactic medium heating from outflows should produce spectral distortions in the cosmic microwave background that will be measurable with the next generation of experiments.

  19. Formation of the wide asynchronous binary asteroid population

    SciTech Connect (OSTI)

    Jacobson, Seth A. [Department of Astrophysical and Planetary Science, UCB 391, University of Colorado, Boulder, CO 80309 (United States); Scheeres, Daniel J.; McMahon, Jay [Department of Aerospace Engineering Sciences, UCB 429, University of Colorado, Boulder, CO 80309 (United States)

    2014-01-01

    We propose and analyze a new mechanism for the formation of the wide asynchronous binary population. These binary asteroids have wide semimajor axes relative to most near-Earth and main belt asteroid systems. Confirmed members have rapidly rotating primaries and satellites that are not tidally locked. Previously suggested formation mechanisms from impact ejecta, from planetary flybys, and directly from rotational fission events cannot satisfy all of the observations. The newly hypothesized mechanism works as follows: (1) these systems are formed from rotational fission, (2) their satellites are tidally locked, (3) their orbits are expanded by the binary Yarkovsky-O'Keefe-Radzievskii-Paddack (BYORP) effect, (4) their satellites desynchronize as a result of the adiabatic invariance between the libration of the secondary and the mutual orbit, and (5) the secondary avoids resynchronization because of the YORP effect. This seemingly complex chain of events is a natural pathway for binaries with satellites that have particular shapes, which define the BYORP effect torque that acts on the system. After detailing the theory, we analyze each of the wide asynchronous binary members and candidates to assess their most likely formation mechanism. Finally, we suggest possible future observations to check and constrain our hypothesis.

  20. Stellar signatures of AGN-jet-triggered star formation

    SciTech Connect (OSTI)

    Dugan, Zachary; Silk, Joseph; Bryan, Sarah; Gaibler, Volker; Haas, Marcel

    2014-12-01

    To investigate feedback between relativistic jets emanating from active galactic nuclei and the stellar population of the host galaxy, we analyze the long-term evolution of the orbits of the stars formed in the galaxy-scale simulations by Gaibler et al. of jets in massive, gas-rich galaxies at z ? 2-3. We find strong, jet-induced differences in the resulting stellar populations of galaxies that host relativistic jets and galaxies that do not, including correlations in stellar locations, velocities, and ages. Jets are found to generate distributions of increased radial and vertical velocities that persist long enough to effectively augment the stellar structure of the host. The jets cause the formation of bow shocks that move out through the disk, generating rings of star formation within the disk. The bow shock often accelerates pockets of gas in which stars form, yielding populations of stars with significant radial and vertical velocities, some of which have large enough velocities to escape the galaxy. These stellar population signatures can serve to identify past jet activity as well as jet-induced star formation.