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Sample records for nova scotia department

  1. Nova Scotia Department of Energy's "Nova Scotia Energy Strategy -Progress Report II"

    E-Print Network [OSTI]

    Hughes, Larry

    Review of Nova Scotia Department of Energy's "Nova Scotia Energy Strategy - Progress Report II" Larry Hughes Energy Research Group Department of Electrical and Computer Engineering Dalhousie University 30 April 2004 Abstract Early in March 2004, the Nova Scotia Department of Energy released its

  2. An Examination of Nova Scotia Power Incorporated's

    E-Print Network [OSTI]

    Hughes, Larry

    1 An Examination of Nova Scotia Power Incorporated's Green Power Rider Larry Hughes Department (NSPI) made application to the Nova Scotia Utility and Review Board for an Optional Green Power Rider to be added to their existing Domestic (that is, residential) Services Rates [1]. The proposed Green Power

  3. Energy Security in Nova Scotia Larry Hughes

    E-Print Network [OSTI]

    Hughes, Larry

    of energy) PV ­ Photovoltaic (usually solar panels that generate electricity from the sun) RES ­ RenewableERG/200703 Energy Security in Nova Scotia Larry Hughes Energy Research Group Department: Energy Security in Nova Scotia 1 Glossary b/d ­ barrels per day BCF ­ Billion Cubic Feet CAPP ­ Canadian

  4. Efficiency Nova Scotia Releases Energy Efficiency Mobile App | Department

    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:FinancingPetroleum Based|DepartmentStatementofApril 25,EVthe nextofof Energy Efficiency Nova

  5. Dendrochronological dating of coal mine workings at the Joggins Fossil Cliffs, Nova Scotia, Canada

    E-Print Network [OSTI]

    Walters, Bradley B.

    Dendrochronological dating of coal mine workings at the Joggins Fossil Cliffs, Nova Scotia, Canada, New Brunswick E4L 1A7, Canada 2. Department of Earth Sciences, Royal Holloway, University of London, Nova Scotia B3H 4J1, Canada * Corresponding author Date received 4 May 2010 ¶ Date

  6. Efficiency Nova Scotia Releases Energy Efficiency Mobile App...

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

    chairs, and a window looking outside. Better Buildings Residential Network member Efficiency Nova Scotia recently released Spot it-an energy efficiency game app for mobile...

  7. NSUARB -NSPI -P-887 NOVA SCOTIA UTILITY AND REVIEW BOARD

    E-Print Network [OSTI]

    Hughes, Larry

    it to purchase electricity from out-of-province suppliers such as NB Power or Quebec Hydro. These higher costs ADJUSTMENT MECHANISM (FAM) FOR NOVA SCOTIA POWER INCORPORATED Comments on FAM Proposals Filed 5 March 2007 Background Unlike most other Canadian utilities, Nova Scotia Power Incorporated relies on fossil energy

  8. Nova Scotia Research and Innovation Graduate Scholarships Information Sheet May 2014

    E-Print Network [OSTI]

    · ICT · Life Sciences · Ocean Science and Tecnology #12;Nova Scotia Research and Innovation Graduate

  9. Towards a new energy strategy for Nova Scotia Response to

    E-Print Network [OSTI]

    Hughes, Larry

    Halifax, Nova Scotia, Canada larry.hughes@dal.ca http://lh.ece.dal.ca/enen 19 December 2007 Natural gas RPP Coal (imp) Coal (dom) Renewables (non-utility) Secure Low carbon High carbon Insecure #12

  10. Energy Security in Nova Scotia Larry Hughes

    E-Print Network [OSTI]

    Hughes, Larry

    ;Energy security: Examples · UK: ­ North Sea oil and natural gas have peaked ­ Relying on Russia (pipeline.3% Coal 25.1% Natural gas 20.9% Biomass 10.6% Nuclear 6.5% Hydro 2.2% Other 0.4% · Energy: ­ Over 98, Saskatchewan, Newfoundland · Natural gas: ­ B.C., Alberta, Saskatchewan, Frontier · Coal: ­ B.C., Alberta, Nova

  11. An Analysis of Likely Scalants in the Treatment of Produced Water from Nova Scotia

    E-Print Network [OSTI]

    Theil, Gregory P.

    A significant barrier to further use of hydraulic fracturing to recover shale oil and/or gas is the treatment and/or disposal of hypersaline produced water. This work is an analysis of produced water from Nova Scotia, with ...

  12. Space Heating Trends in Prince Edward Island and Nova Scotia1 Mandeep Dhaliwal and Larry Hughes

    E-Print Network [OSTI]

    Hughes, Larry

    ERG/200604 Space Heating Trends in Prince Edward Island and Nova Scotia1 Mandeep Dhaliwal and Larry in a northern country such as Canada. Residential space heating is of particular interest in Prince Edward (NRCan) suggests that despite their similarities, the space heating requirements for Prince Edward Island

  13. Does Nova Scotia have an electric future? Response to

    E-Print Network [OSTI]

    Hughes, Larry

    and radical changes in energy markets (IEA, 2007a; NPC, 2007). The cost and availability of crude oil, and electricity (IEA, 2007b). Jurisdictions that rely on supplies of crude oil, coal, and natural gas will be particularly vulnerable to cost increases and supply shortfalls (IEA, 2007b). One such jurisdiction is Nova

  14. Acadia University Wolfville, Nova Scotia BOP 1XO

    E-Print Network [OSTI]

    McLeod, Ian

    : · Chawla, J.S. (1988), A Note on General Ridge Estimator. Communications in Statistics A, 17. #12;2 ACADIA, Multivariate Analysis, Em- pirical Bayes Theory, Distribution Theory, Statistical Modelling, Robust Inference Department offers an undergraduate degree (Honours or general) in statistics. Students are trained in the use

  15. Chronology and stratigraphy of the Fundy and related Nova Scotia offshore basins and Morocco based on core

    E-Print Network [OSTI]

    Olsen, Paul E.

    #12;51 Chronology and stratigraphy of the Fundy and related Nova Scotia offshore basins and Morocco and provided a basis for the development of a complete lithological and paleomagnetic reversal stratigraphy for the Blomidon Formation (Kent and Olsen, 2000). The paleomagnetic polarity stratigraphy of the outcropping

  16. NOVA SCOTIA UTILITY AND REVIEW BOARD IN THE MATTER OF: The Public Utilities Act, R.S.N.S. 1989, c.380 as

    E-Print Network [OSTI]

    Hughes, Larry

    Halifax, Nova Scotia, B3J 2X4, Canada larry.hughes@dal.ca 24 November 2004 Abstract Energy suppliers-subsidization, and does not allow the energy supplier to create price signals. Although other, more progressive billing schemes, such as time-of-usage billing, exist, some energy suppliers and their customers are reluctant

  17. Dalhousie Medical School Cancer Researcher Seeks Biomarkers of Treatment Success HALIFAX,NOVA SCOTIA | CANADA B3H 4H7 | +1 (902) 494-2756

    E-Print Network [OSTI]

    Dellaire, Graham

    ,NOVA SCOTIA | CANADA B3H 4H7 | +1 (902) 494-2756 FACULTY OF MEDICINE COMMUNICATIONS OFFICE NEWS & FEATURE are like the canary in the coal mine, alerting us to potentially cancer-causing changes in the cell and testing biomarkers for early detection of cancer in Atlantic Canada. "My work to locate biomarkers

  18. NOVA SCOTIA UTILITY AND REVIEW BOARD IN THE MATTER OF: The Public Utilities Act, R.S.N.S. 1989, c.380 as

    E-Print Network [OSTI]

    Hughes, Larry

    itself differently from the Independent Power Producers who were competing for11 contracts.12 I have also.S.N.S. 1989, c.380 as amended - and - IN THE MATTER OF: An Application by Nova Scotia Power Incorporated of the7 provincial legislature.8 I have also examined NSPI's Green Power Rider, which was subsequently

  19. Text and slides of presentation originally presented to the Nova Scotia Utility and Review Board regarding the province's Demand Side Management program,19 April 2010.

    E-Print Network [OSTI]

    Hughes, Larry

    households, heats his home with oil (Nova Scotia Finance 2007). When we discussed the issue of oil sources (APERC 2007, Hughes and Shupe 2010). We now live in an age of rising competition for oil products: China and other emerging market economies are increasing their consumption of oil at breathtaking speed

  20. Air Quality (Nova Scotia, Canada) | Department of Energy

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

    Industrial Investor-Owned Utility Multi-Family Residential MunicipalPublic Utility Rural Electric Cooperative Utility Program Info Program Type Environmental Regulations Provider...

  1. EA-355 Scotia Capital Energy, Inc. | 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 GasAdjustmentsShirleyEnergy A plug-inPPL EnergyPlus, LLC to exportEndure Energy, L.L.C. to export electricScotia

  2. Graphics Interface Conference 2015, 35 June, Halifax, Nova Scotia, Canada Penny Pincher: A Blazing Fast, Highly Accurate $-Family Recognizer

    E-Print Network [OSTI]

    Pattanaik, Sumanta N.

    Penny Pincher: A Blazing Fast, Highly Accurate $-Family Recognizer Eugene M. Taranta II Department in certain cases. Our recognizer Penny Pincher achieves high accuracy by being able to process a large number outperform its rival recognizers. Penny Pincher achieves this goal by reducing the template matching process

  3. Toll free 1-877-867-StFX(7839) PO Box 5000, Antigonish, Nova Scotia, Canada B2G 2W5

    E-Print Network [OSTI]

    .6 Admission from Other Systems of Education 4 1.7 Admission to the Bachelor of Science in Nursing 4 1 of Education Professional Conduct 22 6.6 BachelorofEducationCertification 22 6.7 Diploma in Adult Education 22. Department and Programs ................................30 9.1 Adult Education 30 9.2 Anthropology 30 9

  4. EIS-0339: Presidential Permit Application, GenPower 500 kV Submarine Electric Transmission Cable from Nova Scotia to New York

    Broader source: Energy.gov [DOE]

    The Department of Energy (DOE) announced its intent to prepare an Environmental Impact Statement (EIS) in accordance with the National Environmental Policy Act of 1969 (NEPA) for GenPower New York, L.L.C.’s (GenPower) request for a Presidential permit for a proposed international electric transmission line.

  5. Tax Credits, Rebates & Savings | Department of Energy

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

    Community Feed-in Tariff (Nova Scotia, Canada) The Community Feed-In Tariff Program (COMFIT) is designed to increase local ownership of small-scale energy projects in Nova Scotia....

  6. Nova Scotia: 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:QAsource History ViewMayo, Maryland:NPI VenturesNewSt. Louis, Minnesota: EnergyOhio: EnergyNottingham,

  7. Professor Paul S. Hill Department of Oceanography, Dalhousie University, Halifax, Nova Scotia, Canada B3H 4J1

    E-Print Network [OSTI]

    Taggart, Christopher

    /OETR Nearfield effects of tidal power 2009-2012 $208,344 U. S. ONR OASIS II 2010-2011 $142,000 OEER/OETR Farfield effects of tidal power generation 2006-2011: $134,500 NSERC Discovery Oil-mineral aggregation in coastal in the Bay of Fundy #12;2010-2012 $109,329 U. S. ONR Tidal Flats DRI II 2010-2012 $182,300 OEER

  8. Radiological Scoping Survey of the Scotia Depot, Scotia, NY

    SciTech Connect (OSTI)

    Bailey, E. N.

    2008-02-25

    The objectives of the radiological scoping survey were to collect adequate field data for use in evaluating the radiological condition of Scotia Depot land areas, warehouses, and support buildings.

  9. Application to Export Electric Energy OE Docket No. EA-355 Scotia...

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

    Scotia Capital Energyto export electric energy to Canada Application to Export Electric Energy OE Docket No EA-355 Scotia Capital Energy More Documents & Publications EA-355 Scotia...

  10. Surviving racism: African Nova Scotian women talk about the daily

    E-Print Network [OSTI]

    Brownstone, Rob

    Surviving racism: African Nova Scotian women talk about the daily racism they've experienced a discussion Wednesday as part of Dalhousie's Global Health Rounds. Titled "Surviving Racism and its Impact Scotia #12;does not still have a history of racism and I can assure you that that history is strong

  11. Securing our energy future? A review of Nova Scotia's energy sector in 2004

    E-Print Network [OSTI]

    Hughes, Larry

    " .......................................................................................... 7 1.4. Liquefied Natural Gas ...........................................................................................4 1. Natural Gas .............................................................................................20 List of figures and tables Figure 1: Monthly offshore natural gas production to May 2005

  12. Freezing in the dark: Energy security and heating emergencies in Nova Scotia

    E-Print Network [OSTI]

    Hughes, Larry

    · Demand side management · Natural gas · Wind and tidal · Grid upgrade · Lower Churchill #12;What Canada, Survey of Household Spending in 2005, 2005 #12;Cost of fuel by quintile 0% 5% 10% 15% 20% 25 assistance programs: ­ "Your energy rebate" ­ Heating Assistance Rebate Program (HARP) ­ Heat Smart

  13. Response to P-887 Adoption of a Fuel Adjustment Mechanism (FAM) for Nova Scotia Power Incorporated

    E-Print Network [OSTI]

    Hughes, Larry

    as estimated by utility Less than estimated Higher than estimated Consumer Pays more per unit of electricity in the price of electricity paid by the consumer. Rather than periodic rate cases, the utility passes fuels companies, regulated utilities are often intended to set rates that will remain in effect for lengthy

  14. Assessing Success in Aquaculture from the Farmer Perspective: The Case of Nova Scotia, Canada

    E-Print Network [OSTI]

    Charles, Anthony

    (Statistics Canada, 2003). Prince Edward Island in the past 25 years has developed a cultivated mussel

  15. MHK Projects/OpenHydro Bay of Fundy Nova Scotia CA | Open Energy

    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:QAsource History View NewTexas:Montezuma,Information MHKMHK5 < MHK ProjectsHawaiiInformation Bay of Fundy

  16. Nucleosynthesis in classical novae

    E-Print Network [OSTI]

    M. Hernanz; J. Jose; A. Coc

    2001-01-19

    A general review of the relevance of classical novae for the chemical evolution of the Galaxy, as well as for Galactic radioactivity is presented. A special emphasis is put on the pioneering work done by Jim Truran in this field of research. The impact of recent developments in nuclear astrophysics on nova nucleosynthesis, together with the prospects for observability of novae radioactivities with the INTEGRAL satellite are discussed.

  17. Evolution of the Deep and Bottom Waters of the Scotia Sea, Southern Ocean, during 19952005*

    E-Print Network [OSTI]

    Johnson, Gregory C.

    Evolution of the Deep and Bottom Waters of the Scotia Sea, Southern Ocean, during 1995 the eastern Scotia Sea occupied in 1995, 1999, and 2005 reveals significant variability in the deep and bottom 1995 and 1999 reversed through to 2005, reflecting changes seen earlier upstream in the Weddell Sea

  18. On the last mile : the effects of telecommunications regulation and deregulation in the rural western United States and Canada

    E-Print Network [OSTI]

    Kozak, Nadine Irène

    2010-01-01

    Atlantic Provinces are Prince Edward Island, Nova Scotia,Nova Scotia, Prince Edward Island, and Newfoundland and

  19. On the last mile : the effects of telecommunications regulation and deregulation in the rural western United States and Canada

    E-Print Network [OSTI]

    Kozak, Nadine Irène

    2010-01-01

    Provinces are Prince Edward Island, Nova Scotia, and NewNova Scotia, Prince Edward Island, and Newfoundland and

  20. MONITORING STRATIFICATION AND CURRENTS AT THE CONTINENTAL SLOPE OF THE SCOTIA SEA, ANTARCTICA 

    E-Print Network [OSTI]

    Thornton, Melanie 1989-

    2011-05-02

    fulfillment of the requirements for the designation as UNDERGRADUATE RESEARCH SCHOLAR A Senior Scholars Thesis by MELANIE R. THORNTON MONITORING STRATIFICATION AND CURRENTS AT THE CONTINENTAL SLOPE OF THE SCOTIA SEA, ANTARCTICA Approved by... of the requirements for the designation as UNDERGRADUATE RESEARCH SCHOLAR A Senior Scholars Thesis by MELANIE R. THORNTON iii ABSTRACT Monitoring Stratification and Currents at the Continental Slope of the Scotia Sea, Antarctica. (April 2011...

  1. Final Scientific/Technical Report to the U.S. Department of Energy on NOVA's Einstein's Big Idea (Project title: E-mc2, A Two-Hour Television Program on NOVA)

    SciTech Connect (OSTI)

    Susanne Simpson

    2007-05-07

    Executive Summary A woman in the early 1700s who became one of Europe’s leading interpreters of mathematics and a poor bookbinder who became one of the giants of nineteenth-century science are just two of the pioneers whose stories NOVA explored in Einstein’s Big Idea. This two-hour documentary premiered on PBS in October 2005 and is based on the best-selling book by David Bodanis, E=mc2: A Biography of the World’s Most Famous Equation. The film and book chronicle the scientific challenges and discoveries leading up to Einstein’s startling conclusion that mass and energy are one, related by the formula E = mc2.

  2. AT Cnc: A SECOND DWARF NOVA WITH A CLASSICAL NOVA SHELL Shara...

    Office of Scientific and Technical Information (OSTI)

    and that at least some classical novae become dwarf novae long after their nova thermonuclear outbursts, in accord with the hibernation scenario of cataclysmic binaries. Here...

  3. Projected impacts of climate change on species distribution in the Acadian Forest region of eastern Nova Scotia

    E-Print Network [OSTI]

    .e., hydrological cycle and earth- sun geometry. Growing degree days and mean air temperature are basedProjected impacts of climate change on species distribution in the Acadian Forest region of eastern on processing remote sensing data, mean air temperatures serves as one of several inputs to model calculation

  4. Evolution of the Deep and Bottom Waters of the Scotia Sea, Southern Ocean, during 19952005*

    E-Print Network [OSTI]

    Naveira Garabato, Alberto

    Evolution of the Deep and Bottom Waters of the Scotia Sea, Southern Ocean, during 1995. The volume of deep waters with potential temperature less than 0°C decreased during 1995­2005, though. These changes are best explained by interannual variations in the deep waters exiting the Weddell Sea

  5. Argonne's Vilas Pol on NOVA!

    ScienceCinema (OSTI)

    None

    2013-04-19

    Can innovations in materials science help clean up our world? Argonne's material scientist Vilas Pol guest starred on NOVA's "Making Stuff: Cleaner," where David Pogue explored the rapidly-developing science and business of clean energy.

  6. NOvA Experiment - The Local Community

    ScienceCinema (OSTI)

    Deb Wieber

    2010-01-08

    Local proprietors Steve and Deb Wieber discuss the impact of the NOvA experiment on their community.

  7. Personal Health Information Act (PHIA) and Research

    E-Print Network [OSTI]

    Brownstone, Rob

    Personal Health Information Act (PHIA) and Research Dalhousie Research Ethics Board Presented Information Act ­ Provincial privacy legislation under the Nova Scotia Department of Health and Wellness health information for planning or research. · Follows the pattern of protection adopted by various

  8. NOVA Making Stuff Season 2

    SciTech Connect (OSTI)

    Leombruni, Lisa; Paulsen, Christine Andrews

    2014-12-12

    Over the course of four weeks in fall 2013, 11.7 million Americans tuned in to PBS to follow host David Pogue as he led them in search of engineering and scientific breakthroughs poised to change our world. Levitating trains, quantum computers, robotic bees, and bomb-detecting plants—these were just a few of the cutting-edge innovations brought into the living rooms of families across the country in NOVA’s four-part series, Making Stuff: Faster, Wilder, Colder, and Safer. Each of the four one-hour programs gave viewers a behind-the-scenes look at novel technologies poised to change our world—showing them how basic research and scientific discovery can hold the keys to transforming how we live. Making Stuff Season 2 (MS2) combined true entertainment with educational value, creating a popular and engaging series that brought accessible science into the homes of millions. NOVA’s goal to engage the public with such technological innovation and basic research extended beyond the broadcast series, including a variety of online, educational, and promotional activities: original online science reporting, web-only short-form videos, a new online quiz-game, social media engagement and promotion, an educational outreach “toolkit” for science educators to create their own “makerspaces,” an online community of practice, a series of nationwide Innovation Cafés, educator professional development, a suite of teacher resources, an “Idealab,” participation in national conferences, and specialized station relation and marketing. A summative evaluation of the MS2 project indicates that overall, these activities helped make a significant impact on the viewers, users, and participants that NOVA reached. The final evaluation conducted by Concord Evaluation Group (CEG) confidently concluded that the broadcast, website, and outreach activities were successful at achieving the project’s intended impacts. CEG reported that the MS2 series and website content were successful in raising awareness and sparking interest in innovation, and increased public awareness that basic research leads to technological innovation; this interest was also sustained over a six month period. Efforts to create an online community of practice were also successful: the quality of collaboration increased, and community members felt supported while using Maker pedagogy. These findings provide clear evidence that large-scale science media projects like MS2 are an effective means of “moving the needle” on attitudes about and excitement for science. NOVA’s broadcast audience and ratings have always indicated that a large portion of the population is interested in and engages with educational science media on a weekly basis. Yet these evaluation results provide the empirical evidence that beyond being capable of attracting, maintaining, and growing a dedicated group of citizens interested in science, these shows—with their diverse content provided on a variety of media channels—are capable of sparking new interest in science, raising public awareness of the importance of science, and maintaining and growing that interest over time. In a country where approximately a quarter of the population doesn’t know the earth rotates around the sun,1 roughly half still don’t accept evolution,2 and about 20% don’t think climate change is happening,3 the importance of these findings cannot be overstated. The success of MS2 suggests that large-scale media projects dedicated to and linked by coverage of scientific “big ideas” are an effective means of shifting public opinion on—and improving understanding of—science. REFERENCES 1, 2 National Science Foundation, Science and Engineering Indicators (2014). Chapter 7: Science and Technology: Public Attitudes and Understanding. 3 Leiserowitz, A., Maibach, E., Roser-Renouf, C., Feinberg, G., & Rosenthal, S. (2014) Climate change in the American mind: April, 2014. Yale University and George Mason University. New Haven, CT: Yale Project on Climate Change Communication.

  9. Hopkins Ultraviolet Telescope Observations of Nova Circini 1995 and Nova Aquilae 1995

    E-Print Network [OSTI]

    Hopkins Ultraviolet Telescope Observations of Nova Circini 1995 and Nova Aquilae 1995 Bradford W 1995 and Nova Aql 1995 with the Hopkins Ultraviolet Telescope during the Astro­2 space shuttle mission in 1995 March. The spectra cover the wavelength range from 820 š A to 1840 š A with a spectral resolution

  10. NOVA Portal: Submit VASP Jobs to Carver via the Web

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

    NOVA Portal: Submit VASP Jobs to Carver via the Web NOVA Portal: Submit VASP Jobs to Carver via the Web May 11, 2012 by Francesca Verdier NOVA is an experimental web application...

  11. Title: Canadian Soil Information System (CanSIS) Data Creator /

    E-Print Network [OSTI]

    , Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon

  12. Title: Canada Land Inventory: Land Capability for Recreation Data Creator /

    E-Print Network [OSTI]

    and Labrador, Nova Scotia, Ontario, Prince Edward Island, Quebec, Saskatchewan Keywords (Subject): Lakes

  13. library.dal.ca University Archives &

    E-Print Network [OSTI]

    Lotze, Heike K.

    and shipping registers from Nova Scotia, New Brunswick and Prince Edward Island. special collections features

  14. Title: ArcCanada 3.0: National Data Data Creator /

    E-Print Network [OSTI]

    , Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon #12

  15. Title: Surficial Materials of Canada (Map 1880A) Data Creator /

    E-Print Network [OSTI]

    Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon Keywords

  16. Title: CanVec Data Creator /

    E-Print Network [OSTI]

    Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon #12;Keywords

  17. Title: CanMatrix Data Creator /

    E-Print Network [OSTI]

    and Labrador, Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan

  18. Title: Enhanced Points of Interest: Canada Data Creator /

    E-Print Network [OSTI]

    Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon #12;Keywords

  19. Title: Platinum Postal Suite Local Delivery Unit (LDU): Canada Data Creator /

    E-Print Network [OSTI]

    , Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan, Yukon

  20. Title: Canada Land Inventory: Land Capability for Waterfowl Wildlife Data Creator /

    E-Print Network [OSTI]

    , Newfoundland and Labrador, Nova Scotia, Ontario, Prince Edward Island, Quebec, Saskatchewan Keywords (Subject

  1. Title: Landsat 7 Orthorectified Imageries over Canada Data Creator /

    E-Print Network [OSTI]

    , Newfoundland and Labrador, Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec

  2. For Immediate Release April 7, 2015

    E-Print Network [OSTI]

    Law, Wayne

    with provincial and federal governments in Nova Scotia, Prince Edward Island, and several other Canadian provinces

  3. Title: GeoPinpoint Suite Data Creator /

    E-Print Network [OSTI]

    and Labrador, Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince Edward Island, Quebec, Saskatchewan

  4. Near Infrared studies during maximum and early decline of Nova Cephei 2014 and Nova Scorpii 2015

    E-Print Network [OSTI]

    Srivastava, Mudit K; Banerjee, D P K; Sand, D

    2015-01-01

    We present multi-epoch near-infrared photo-spectroscopic observations of Nova Cephei 2014 and Nova Scorpii 2015, discovered in outburst on 2014 March 8.79 UT and 2015 February 11.84 UT respectively. Nova Cep 2014 shows the conventional NIR characteristics of a Fe II class nova characterized by strong CI, HI and O I lines, whereas Nova Sco 2015 is shown to belong to the He/N class with strong He I, HI and OI emission lines. The highlight of the results consists in demonstrating that Nova Sco 2015 is a symbiotic system containing a giant secondary. Leaving aside the T CrB class of recurrent novae, all of which have giant donors, Nova Sco 2015 is shown to be only the third classical nova to be found with a giant secondary. The evidence for the symbiotic nature is three-fold; first is the presence of a strong decelerative shock accompanying the passage of the nova's ejecta through the giant's wind, second is the H$\\alpha$ excess seen from the system and third is the spectral energy distribution of the secondary i...

  5. Shortest recurrence periods of novae

    SciTech Connect (OSTI)

    Kato, Mariko [Department of Astronomy, Keio University, Hiyoshi, Yokohama 223-8521 (Japan); Saio, Hideyuki [Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578 (Japan); Hachisu, Izumi [Department of Earth Science and Astronomy, College of Arts and Sciences, The University of Tokyo, 3-8-1 Komaba, Meguro-ku, Tokyo 153-8902 (Japan); Nomoto, Ken'ichi, E-mail: mariko@educ.cc.keio.ac.jp [Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan)

    2014-10-01

    Stimulated by the recent discovery of the 1 yr recurrence period nova M31N 2008-12a, we examined the shortest recurrence periods of hydrogen shell flashes on mass-accreting white dwarfs (WDs). We discuss the mechanism that yields a finite minimum recurrence period for a given WD mass. Calculating the unstable flashes for various WD masses and mass accretion rates, we identified a shortest recurrence period of about two months for a non-rotating 1.38 M {sub ?} WD with a mass accretion rate of 3.6 × 10{sup –7} M {sub ?} yr{sup –1}. A 1 yr recurrence period is realized for very massive (? 1.3 M {sub ?}) WDs with very high accretion rates (? 1.5 × 10{sup –7} M {sub ?} yr{sup –1}). We revised our stability limit of hydrogen shell burning, which will be useful for binary evolution calculations toward Type Ia supernovae.

  6. The NOvA Technical Design Report

    SciTech Connect (OSTI)

    Ayres, D.S.; Drake, G.R.; Goodman, M.C.; Grudzinski, J.J.; Guarino, V.J.; Talaga, R.L.; Zhao, A.; Stamoulis, P.; Stiliaris, E.; Tzanakos, G.; Zois, M.; /Athens U. /Caltech /UCLA /Fermilab /College de France /Harvard U. /Indiana U. /Lebedev Inst. /Michigan State U. /Minnesota U., Duluth /Minnesota U.

    2007-10-08

    Technical Design Report (TDR) describes the preliminary design of the NOvA accelerator upgrades, NOvA detectors, detector halls and detector sites. Compared to the March 2006 and November 2006 NOvA Conceptual Design Reports (CDR), critical value engineering studies have been completed and the alternatives still active in the CDR have been narrowed to achieve a preliminary technical design ready for a Critical Decision 2 review. Many aspects of NOvA described this TDR are complete to a level far beyond a preliminary design. In particular, the access road to the NOvA Far Detector site in Minnesota has an advanced technical design at a level appropriate for a Critical Decision 3a review. Several components of the accelerator upgrade and new neutrino detectors also have advanced technical designs appropriate for a Critical Decision 3a review. Chapter 1 is an Executive Summary with a short description of the NOvA project. Chapter 2 describes how the Fermilab NuMI beam will provide a narrow band beam of neutrinos for NOvA. Chapter 3 gives an updated overview of the scientific basis for the NOvA experiment, focusing on the primary goal to extend the search for {nu}{sub {mu}} {yields} {nu}{sub e} oscillations and measure the sin{sup 2}(2{theta}{sub 13}) parameter. This parameter has not been measured in any previous experiment and NOvA would extend the search by about an order of magnitude beyond the current limit. A secondary goal is to measure the dominant mode oscillation parameters, sin{sup 2}(2{theta}{sub 23}) and {Delta}m{sub 32}{sup 2} to a more precise level than previous experiments. Additional physics goals for NOvA are also discussed. Chapter 4 describes the Scientific Design Criteria which the Fermilab accelerator complex, NOvA detectors and NOvA detector sites must satisfy to meet the physics goals discussed in Chapter 3. Chapter 5 is an overview of the NOvA project. The changes in the design relative to the NOvA CDR are discussed. Chapter 6 summarizes the NOvA design performance relative to the Design Criteria set out in Chapter 4. Chapter 7 presents the Work Breakdown Structure dictionary at Level 3 and the Milestone dictionary. Chapters 8 through 17 then take each Level 2 WBS element of the NOvA project and present each part of the design in more detail than the overview given in Chapter 5. Specific technical design criteria are delineated for each part of the project in addition to the scientific design criteria outlined in Chapter 4. Changes in the design since the NOvA CDR are discussed in detail. The work remaining to bring each part of this preliminary design to a final design is outlined. Appendix A is a guide to other NOvA Project documentation with links to those documents.

  7. WZ Sge-Type Dwarf Novae

    E-Print Network [OSTI]

    Kato, Taichi

    2015-01-01

    We have summarized the current understanding and recently obtained findings about WZ Sge-type dwarf novae. We also reviewed the historical development of the understanding of these objects, provided the modern criteria, and reviewed the past research in relation to superhumps, early superhumps and the outburst mechanism. We regard that the presence of early superhumps (reflecting the 2:1 resonance) and long or multiple rebrightenings are the best distinguishing properties of WZ Sge-type dwarf novae. We provided the updated list of nearly 100 WZ Sge-type dwarf novae mainly based on the data obtained by the VSNET Collaboration up to Kato et al. (2015, arXiv/1507.05610) and discussed the statistics. We could detect early superhumps with amplitude larger than 0.02 mag in 63% of the studied WZ Sge-type dwarf novae, which makes early superhumps a useful distinguishing feature for WZ Sge-type dwarf novae. Theoretical light curves of early superhumps generally appear to reproduce the existence of many low-amplitude o...

  8. The Expanding Fireball of Nova Delphini 2013

    E-Print Network [OSTI]

    Schaefer, G H; Gies, D R; Farrington, C D; Kloppenborg, B; Chesneau, O; Monnier, J D; Ridgway, S T; Scott, N; Tallon-Bosc, I; McAlister, H A; Boyajian, T; Maestro, V; Mourard, D; Meilland, A; Nardetto, N; Stee, P; Sturmann, J; Vargas, N; Baron, F; Ireland, M; Baines, E K; Che, X; Jones, J; Richardson, N D; Roettenbacher, R M; Sturmann, L; Turner, N H; Tuthill, P; van Belle, G; von Braun, K; Zavala, R T; Banerjee, D P K; Ashok, N M; Joshi, V; Becker, J; Muirhead, P S

    2015-01-01

    A classical nova occurs when material accreting onto the surface of a white dwarf in a close binary system ignites in a thermonuclear runaway. Complex structures observed in the ejecta at late stages could result from interactions with the companion during the common envelope phase. Alternatively, the explosion could be intrinsically bipolar, resulting from a localized ignition on the surface of the white dwarf or as a consequence of rotational distortion. Studying the structure of novae during the earliest phases is challenging because of the high spatial resolution needed to measure their small sizes. Here we report near-infrared interferometric measurements of the angular size of Nova Delphini 2013, starting from one day after the explosion and continuing with extensive time coverage during the first 43 days. Changes in the apparent expansion rate can be explained by an explosion model consisting of an optically thick core surrounded by a diffuse envelope. The optical depth of the ejected material changes ...

  9. Fermilab | Newsroom | Press Releases | March 2013: NOvA Photos

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

    NOvA collaboration. Med Res | Hi Res The NOvA detector, currently under construction in Ash River, Minn., stands about 50 feet tall and 50 feet wide. The completed detector will...

  10. Fermilab | Newsroom | Press Releases | February 2014: NOvA Images

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

    NOvA collaboration Med Res | Hi Res The NOvA detector, currently under construction in Ash River, Minn., stands about 50 feet tall and 50 feet wide. The completed detector will...

  11. Revista Electrnica Nova Scientia Propagacin temporal de algunas enfermedades

    E-Print Network [OSTI]

    Cipolatti, Rolci

    Revista Electrónica Nova Scientia Propagación temporal de algunas enfermedades bacterianas: un: a mathematical model Revista Electrónica Nova Scientia, Nº 8 Vol. 4 (2), 2012. ISSN 2007 - 0705. pp: 42 - 65 - 43;Cipolatti, R. et al. Revista Electrónica Nova Scientia, Nº 8 Vol. 4 (2), 2012. ISSN 2007 - 0705. pp: 42 ­ 65

  12. NOvA: Exploring Neutrino Mysteries

    ScienceCinema (OSTI)

    Vahle, Tricia; Messier, Mark

    2014-08-12

    Neutrinos are a mystery to physicists. They exist in three different flavors and mass states and may be able to give hints about the origins of the matter-dominated universe. A new long-baseline experiment led by Fermilab called NOvA may provide some answers.

  13. THE DWARF NOVA OUTBURSTS OF NOVA HER 1960 (=V446 HER)

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Robertson, J. W.; Kafka, S. E-mail: jrobertson@atu.edu

    2011-04-15

    V446 Her is the best example of an old nova which has developed dwarf nova (DN) eruptions in the post-nova state. We report on observed properties of the long-term light curve of V446 Her, using photometry over 19 years. Yearly averages of the outburst (OB) magnitudes show a decline of {approx}0.013 mag yr{sup -1}, consistent with the decline of other post-novae that do not have DN OBs. Previous suggestions of bimodal distributions of the amplitudes and widths of the OBs are confirmed. The OBs occur at a mean spacing of 18 days but the range of spacings is large (13-30 days). From simulations of DN OBs, it has been predicted that the OB spacing in V446 Her will increase as M-dot from the red dwarf companion slowly falls following the nova; however, the large intrinsic scatter in the spacings serves to hide any evidence of this effect. We do find a systematic change in the OB pattern in which the brighter, wider type of OBs disappeared after late 2003, and this phenomenon is suggested to be due to falling M-dot following the nova.

  14. The Imprint of Nova Nucleosynthesis in Presolar Grains

    E-Print Network [OSTI]

    Jordi Jose; Margarita Hernanz; Sachiko Amari; Katharina Lodders; Ernst Zinner

    2004-05-17

    Infrared and ultraviolet observations of nova light curves have confirmed grain formation in their expanding shells that are ejected into the interstellar medium by a thermonuclear runaway. In this paper, we present isotopic ratios of intermediate-mass elements up to silicon for the ejecta of CO and ONe novae, based on 20 hydrodynamic models of nova explosions. These theoretical estimates will help to properly identify nova grains in primitive meteorites. In addition, equilibrium condensation calculations are used to predict the types of grains that can be expected in the nova ejecta, providing some hints on the puzzling formation of C-rich dust in O>C environments. These results show that SiC grains can condense in ONe novae, in concert with an inferred (ONe) nova origin for several presolar SiC grains.

  15. Improved optical diagnostics for the NOVA laser

    SciTech Connect (OSTI)

    Fernandez, J.C.; Berggren, R.R.; Bradley, K.S.; Hsing, W.W.; Gomez, C.C.; Cobble, J.A.

    1994-07-01

    This paper describes three diagnostics for detecting optical scatter from NOVA laser targets. Detecting such scatter can help not only the authors` understanding of plasma instabilities in laser plasmas, but also their efforts at plasma characterization, particularly hohlraum plasmas. These diagnostics are: the Full Aperture Backscatter Station (FABS), presently being built; the Oblique Scatter Array (OSA), just starting operation; and the Axial Imager, also just starting operation. FABS will allow imaging at high resolution of Brillouin and Raman backscatter. The OSA allows a quantitative measurement of Brillouin and Raman scatter in many directions (assuming the target allows the scatter to escape). The axial imager allows high-resolution imaging of Brillouin, Two-Plasmon Decay and Raman scatter emitted towards the East direction, which is along the symmetry axis of the NOVA laser beams.

  16. Improved optical diagnostics for the NOVA laser

    SciTech Connect (OSTI)

    Fernandez, J.C.; Berggren, R.R.; Bradley, K.S.; Hsing, W.W.; Gomez, C.C.; Cobble, J.A.; Wilke, M.D. )

    1995-01-01

    This paper describes three diagnostics detecting optical scatter from NOVA laser targets. Detecting such scatter can help to understand instabilities in laser plasmas and to characterize such plasmas, particularly hohlraum plasmas. These diagnostics are the full aperture backscatter station (FABS), presently being built; the oblique scatter array (OSA), just starting operation; and the axial imager, also just starting operation. FABS will allow imaging at high resolution of Brillouin and Raman backscatter. The OSA provides a quantitative measurement of Brillouin and Raman scatter in many directions. The axial imager allows high-resolution imaging of Brillouin, two-plasmon decay and Raman scatter emitted toward the direction of the symmetry axis of the NOVA laser beams.

  17. Hubble Space Telescope Observations of Novae in M49

    E-Print Network [OSTI]

    Laura Ferrarese; Patrick Cote; Andres Jordan

    2003-09-30

    A search for novae in M49 (NGC 4472) has been undertaken with the Hubble Space Telescope. A 55-day observing campaign in F555W (19 epochs) and F814W (five epochs) has led to the discovery of nine novae. We find that M49 may be under-abundant in slow, faint novae relative to the Milky Way and M31. Instead, the decline rates of the M49 novae are remarkably similar to those of novae in the LMC. This fact argues against a simple classification of novae in "bulge" and "disk" sub-classes. We examine the Maximum-Magnitude versus Rate of Decline (MMRD) relation for novae in M49, finding only marginal agreement with the Galactic and M31 MMRD relations. A recalibration of the Buscombe-de Vaucouleurs relation gives an absolute magnitude 15 days past maximum of M_{V,15} = -6.36+/-0.19, which is substantially brighter than previous calibrations based on Galactic novae. Monte Carlo simulations yield a global nova rate for M49 of 100{+35}{-30} per year, and a luminosity-specific nova rate in the range \

  18. Getting to know Classical Novae with Swift

    E-Print Network [OSTI]

    Osborne, Julian P

    2015-01-01

    Novae have been reported as transients for more than two thousand years. Their bright optical outbursts are the result of explosive nuclear burning of gas accreted from a binary companion onto a white dwarf. Novae containing a white dwarf close to the Chandrasekhar mass limit and accreting at a high rate are potentially the unknown progenitors of the type Ia supernovae used to measure the acceleration of the Universe. Swift X-ray observations have radically transformed our view of novae by providing dense monitoring throughout the outburst, revealing new phenomena in the super-soft X-rays from the still-burning white dwarf such as early extreme variability and half- to one-minute timescale quasi-periodic oscillations. The distinct evolution of this emission from the harder X-ray emission due to ejecta shocks has been clearly delineated. Soft X-ray observations allow the mass of the white dwarf, the mass burned and the mass ejected to be estimated. In combination with observations at other wavelengths, includi...

  19. DEFINITIONS Alumni Council

    E-Print Network [OSTI]

    representation of members, consisting of Newfoundland and Labrador, Nova Scotia, New Brunswick, Prince Edward Newfoundland-1; Nova Scotia-4; New Brunswick-2; Prince Edward Island-1; Quebec-1; Ontario-3; Prairies-2

  20. Spectra Nova Technologies Inc | 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| Open Energy Information Serbia-Enhancing CapacityVectren) Jump to: navigation,SouthwoodJump to:NewSpecialSpectra Nova

  1. Api Nova Energia Srl | 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 J APPENDIX E LISTStar Energy LLC Jump to: navigation,Summaries | Open EnergyRoadmap andApi Nova

  2. NovaTorque | 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 J APPENDIXsourceII Jump to:Information 3rd|Northfork Electric Coop, IncUSA(TXR150000)NovaTorque

  3. Petra Nova Project Breaks Ground on World's Largest Post-Combustion...

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

    Petra Nova Project Breaks Ground on World's Largest Post-Combustion Carbon Capture Project Petra Nova Project Breaks Ground on World's Largest Post-Combustion Carbon Capture...

  4. Nuclear Ashes: Reviewing Thirty Years of Nucleosynthesis in Classical Novae

    E-Print Network [OSTI]

    Jordi Jose

    2002-09-10

    One of the observational evidences in support of the "thermonuclear runaway model" for the classical nova outburst relies on the accompanying nucleosynthesis. In this paper, we stress the relevant role played by nucleosynthesis in our understanding of the nova phenomenon by constraining models through a comparison with both the atomic abundance determinations from the ejecta and the isotopic ratios measured in presolar grains of a likely nova origin. Furthermore, the endpoint of nova nucleosynthesis provides hints for the understanding of the mixing process responsible for the enhanced metallicities found in the ejecta, and reveals also information on the properties of the underlying white dwarf (mass, luminosity...). We discuss first the interplay between nova outbursts and the Galactic chemical abundances: Classical nova outbursts are expected to be the major source of 13C, 15N and 17O in the Galaxy, and to contribute to the abundances of other species with A < 40, such as 7Li or 26Al. We describe the main nuclear path during the course of the explosion, with special emphasis on the synthesis of radioactive species, of particular interest for the gamma-ray output predicted from novae (7Li, 18F, 22Na, 26Al). An overview of the recent discovery of presolar nova candidate grains, as well as a discussion of the role played by nuclear uncertainties associated with key reactions of the NeNa-MgAl and Si-Ca regions, are also given.

  5. GUARANTEED ADMISSION AGREEMENT Northern Virginia Community College (NOVA)

    E-Print Network [OSTI]

    Hammack, Richard

    1 GUARANTEED ADMISSION AGREEMENT Between Northern Virginia Community College (NOVA) And Virginia admission agreement (GAA) establishes a collaborative arrangement between NOVA and VCU for the benefit in Liberal Studies for Early and Elementary Education (LSEE) and Master of Teaching degree in Elementary

  6. The NOvA Experiment: Status and Outlook

    E-Print Network [OSTI]

    R. B. Patterson; for the NOvA Collaboration

    2012-09-04

    The NOvA long-baseline neutrino oscillation experiment is currently under construction and will use an upgraded NuMI neutrino source at Fermilab and a 14-kton detector at Ash River, Minnesota to explore the neutrino sector. NOvA uses a highly active, finely segmented detector design that offers superb event identification capability, allowing precision measurements of \

  7. Cimpor inventa nova frmula para reduzir pegada de CO2

    E-Print Network [OSTI]

    Instituto de Sistemas e Robotica

    Cimpor inventa nova fórmula para reduzir pegada de CO2 CIMENTO. A Cimpor descobriu uma nova fórmula para produzir ci- mento que lhe permitirá reduzir a pegada de CO 2 em 25%. Segundo as contas da as fábricas do grupo, seriam emitidos menos quatro milhões de toneladas de CO 2 por ano, o que permitiria uma

  8. Quark Nova Model for Fast Radio Bursts

    E-Print Network [OSTI]

    Zachary Shand; Amir Ouyed; Nico Koning; Rachid Ouyed

    2015-05-29

    FRBs are puzzling, millisecond, energetic radio transients with no discernible source; observations show no counterparts in other frequency bands. The birth of a quark star from a parent neutron star experiencing a quark nova - previously thought undetectable when born in isolation - provides a natural explanation for the emission characteristics of FRBs. The generation of unstable r-process elements in the quark nova ejecta provides millisecond exponential injection of electrons into the surrounding strong magnetic field at the parent neutron star's light cylinder via $\\beta$-decay. This radio synchrotron emission has a total duration of hundreds of milliseconds and matches the observed spectrum while reducing the inferred dispersion measure by approximately 200 cm$^{-3}$ pc. The model allows indirect measurement of neutron star magnetic fields and periods in addition to providing astronomical measurements of $\\beta$-decay chains of unstable neutron rich nuclei. Using this model, we can calculate expected FRB average energies ($\\sim$ 10$^{41}$ ergs), spectra shapes and provide a theoretical framework for determining distances.

  9. Contingent Valuation, Hypothetical Bias and Experimental Economics JAMES J. MURPHY

    E-Print Network [OSTI]

    Murphy, James J.

    of Massachusetts-Amherst Prepared for the NAREA-CAES Conference June 20-23, 2004 Halifax, Nova Scotia Abstract

  10. VALUE OF 1970 LANDINGS IN MARITIME PROVINCES SETS RECORD

    E-Print Network [OSTI]

    s and Forestry. The Maritimes are Nova Scotia, New Brunswick, and Prince Edward Island. Preliminary data show

  11. INCIDENCE OF CULL LOBSTERS, HOMARUS AMERICANUS, IN COMMERCIAL AND RESEARCH CATCHES OFF THE MAINE COASTI

    E-Print Network [OSTI]

    that commercially caught lobsters from ports off Nova Scotia and Prince Edward Island had incidences of missing

  12. TIDAL NOVAE IN COMPACT BINARY WHITE DWARFS

    SciTech Connect (OSTI)

    Fuller, Jim; Lai Dong [Department of Astronomy, Cornell University, Ithaca, NY 14850 (United States)

    2012-09-01

    Compact binary white dwarfs (WDs) undergoing orbital decay due to gravitational radiation can experience significant tidal heating prior to merger. In these WDs, the dominant tidal effect involves the excitation of outgoing gravity waves in the inner stellar envelope and the dissipation of these waves in the outer envelope. As the binary orbit decays, the WDs are synchronized from outside in (with the envelope synchronized first, followed by the core). We examine the deposition of tidal heat in the envelope of a carbon-oxygen WD and study how such tidal heating affects the structure and evolution of the WD. We show that significant tidal heating can occur in the star's degenerate hydrogen layer. This layer heats up faster than it cools, triggering runaway nuclear fusion. Such 'tidal novae' may occur in all WD binaries containing a CO WD, at orbital periods between 5 minutes and 20 minutes, and precede the final merger by 10{sup 5}-10{sup 6} years.

  13. Liquid scintillator production for the NOvA experiment

    E-Print Network [OSTI]

    S. Mufson; B. Baugh; C. Bower; T. E. Coan; J. Cooper; L. Corwin; J. A. Karty; P. Mason; M. D. Messier; A. Pla-Dalmau; M. Proudfoot

    2015-06-30

    The NOvA collaboration blended and delivered 8.8 kt (2.72M gal) of liquid scintillator as the active detector medium to its near and far detectors. The composition of this scintillator was specifically developed to satisfy NOvA's performance requirements. A rigorous set of quality control procedures was put in place to verify that the incoming components and the blended scintillator met these requirements. The scintillator was blended commercially in Hammond, IN. The scintillator was shipped to the NOvA detectors using dedicated stainless steel tanker trailers cleaned to food grade.

  14. THE IMPRINT OF NOVA NUCLEOSYNTHESIS IN PRESOLAR GRAINS Jordi Jose

    E-Print Network [OSTI]

    into the interstellar medium by a thermonuclear runaway. In this paper we present isotopic ratios of intermediate Classical novae are powered by thermonuclear runaways (TNRs) that occur on the white dwarf (WD) component

  15. THE INTER-ERUPTION TIMESCALE OF CLASSICAL NOVAE FROM EXPANSION...

    Office of Scientific and Technical Information (OSTI)

    than 1000 years. The intriguing suggestion that Z Cam was a bright nova, recorded by Chinese imperial astrologers in October-November 77 B.C.E., is consistent more with our...

  16. Fermilab | Newsroom | Press Releases | October 6, 2014: NOvA...

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

    courtesy of Fermilab Med Res | Hi Res A view across the top of the NOvA far detector in Ash River, Minnesota. Electronics that make up part of the data acquisition system are...

  17. The transition phase in Nova Muscae 1998, the dust formation in classical novae and a possible link to intermediate polar systems

    E-Print Network [OSTI]

    A. Retter; W. Liller; G. Garradd

    1999-05-28

    We present results of continuous CCD photometry of Nova Muscae 1998 during 17 nights obtained mainly during the transition phase in the light curve of the young nova. We discovered a periodical oscillation with the period 0.16930 day. This result is important for understanding this peculiar stage in the light curve of certain classical novae. We also note a possible connection between the transition / dust phase in nova light curves and intermediate polar systems.

  18. 361Computer Physics Communications 33(1984) 361 --366 North-Holland, Amsterdam

    E-Print Network [OSTI]

    Creutz, Michael

    1984-01-01

    FOR INVESTIGATIONS ON THE THREE-DIMENSIONAL ISING MODEL Michael CREUTZ Department of Physics, Brookhaven National, Statistics and Computing Science, Daihousie University, Halifax, Nova Scotia B3H 4H8, Canada and K 10 April 1984; in revised form 8 May 1984 PROGRAM SUMMARY Title ofprogram: ISING Keywords: Ising

  19. Winston Roberts Born: 10 September 1958; Port of Spain, Trinidad

    E-Print Network [OSTI]

    McQuade, D. Tyler

    2006 - present · Program Manager, Office of Nuclear Physics, Department of Energy, 2005 (on leave from National Young Investigator Award, 1994. · Natural Sciences and Engineering Research Council of Canada Post University, Halifax, Nova Scotia, Canada, 1979-1983 B. Sc. with Honours in Physics, 1983 · University

  20. Computer Physics Communications 39 (1986) 173--180 173 North-Holland, Amsterdam

    E-Print Network [OSTI]

    Creutz, Michael

    1986-01-01

    FOR THE THREE-DIMENSIONAL ISING MODEL Michael CREUTZ Department of Physics, Brookhaven National Laboratory, Statistics and Computing Science, Daihousie University, Halifax, Nova Scotia B3H 4H8, Canada Received 25 April 1985; in revised form 15 August 1985 PROGRAM SUMMARY Title ofprogram: MICROIS mentary magnets

  1. Petra Nova - W.A. Parish Project | 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 GasAdjustmentsShirleyEnergy AEnergyPresidential PermitDAYS - WE NEED ADr. Peter B. Lyons - AssistantPeterThe

  2. Multi-Dimensional Modeling of Nova with Realistic Nuclear Physics

    SciTech Connect (OSTI)

    Zingale, M; Hoffman, R D

    2011-01-27

    This contract covered the period from 03/09/2010 to 09/30/2010. Over this period, we adapted the low Mach number hydrodynamics code MAESTRO to perform simulations of novae. A nova is the thermonuclear runaway of an accreted hydrogen layer on the surface of a white dwarf. As the accreted layer grows in mass, the temperature and density at the base increase to the point where hydrogen fusion can begin by the CNO cycle - a burning process that uses carbon, nitrogen, and oxygen to complete the fusion of four hydrogen nuclei into one helium-4 nucleus. At this point, we are running initial models of nova, exploring the details of the convection. In the follow-on contract to this one, we will continue this investigation.

  3. nova.tex, 781996. SCATTERING OF LIGHT BY FREE ELECTRONS

    E-Print Network [OSTI]

    Rodriguez, Carlos

    nova.tex, 7­8­1996. SCATTERING OF LIGHT BY FREE ELECTRONS as a Test of Quantum Theory \\Lambda E. T. RELATIVISTIC BASIS OF THE SCHR ¨ ODINGER EQUATION 9 8. NON--ARISTOTELIAN SCATTERING OF LIGHT BY ELECTRONS 10 9 dominates every home and office. But on the other hand, this very fact makes it seem strange that a meeting

  4. CCD Photometry of Nova V1500 Cygni Twenty Years After

    E-Print Network [OSTI]

    I. Semeniuk; A. Olech; M. Nalezyty

    1995-12-14

    We report on CCD photometry of Nova V1500 Cygni obtained in July 1995 to show that twenty years after outburst, being of about 18~mag, the star can still be observed with small telescopes. The 0.1396 day period continues to be stable.

  5. NOvA: Building a Next Generation Neutrino Experiment

    ScienceCinema (OSTI)

    Perko, John; Williams, Ron; Miller, Bill;

    2014-05-30

    The NOvA neutrino experiment is searching for the answers to some of the most fundamental questions of the universe. This video documents how collaboration between government research institutions like Fermilab, academia and industry can create one of the largest neutrino detectors in the world.

  6. VERITAS Observations of the Nova in V407 Cygni

    E-Print Network [OSTI]

    Aliu, E; Arlen, T; Aune, T; Beilicke, M; Benbow, W; Bouvier, A; Bradbury, S M; Buckley, J H; Bugaev, V; Byrum, K; Cannon, A; Cesarini, A; Ciupik, L; Collins-Hughes, E; Connolly, M P; Cui, W; Decerprit, G; Dickherber, R; Duke, C; Dumm, J; Dwarkadas, V V; Errando, M; Falcone, A; Feng, Q; Finley, J P; Finnegan, G; Fortson, L; Furniss, A; Galante, N; Gall, D; Godambe, S; Griffin, S; Grube, J; Gyuk, G; Hanna, D; Holder, J; Huan, H; Hughes, G; Humensky, T B; Kaaret, P; Karlsson, N; Kertzman, M; Khassen, Y; Kieda, D; Krawczynski, H; Krennrich, F; Lang, M J; Lee, K; Maier, G; Majumdar, P; McArthur, S; McCann, A; Millis, J; Moriarty, P; Mukherjee, R; Nuñez, P D; Ong, R A; Orr, M; Otte, A N; Pandel, D; Park, N; Perkins, J S; Pohl, M; Prokoph, H; Quinn, J; Ragan, K; Reyes, L C; Reynolds, P T; Roache, E; Rose, H J; Ruppel, J; Saxon, D B; Schroedter, M; Sembroski, G H; Skole, C; Smith, A W; Staszak, D; Telezhinsky, I; Teši?, G; Theiling, M; Thibadeau, S; Tsurusaki, K; Tyler, J; Varlotta, A; Vincent, S; Vivier, M; Wakely, S P; Ward, J E; Weekes, T C; Weinstein, A; Weisgarber, T; Welsing, R; Williams, D A; Zitzer, B

    2012-01-01

    We report on very high energy (E > 100 GeV) gamma-ray observations of V407 Cygni, a symbiotic binary that underwent a nova outburst producing 0.1-10 GeV gamma rays during 2010 March 10-26. Observations were made with the Very Energetic Radiation Imaging Telescope Array System during 2010 March 19-26 at relatively large zenith angles, due to the position of V407 Cyg. An improved reconstruction technique for large zenith angle observations is presented and used to analyze the data. We do not detect V407 Cygni and place a differential upper limit on the flux at 1.6 TeV of 2.3 \\times 10^(-12) erg cm^(-2) s^(-1) (at the 95% confidence level). When considered jointly with data from Fermi-LAT, this result places limits on the acceleration of very high energy particles in the nova.

  7. On the C/O Enrichment of Novae Ejecta

    E-Print Network [OSTI]

    R. Rosner; A. Alexakis; Y. Young; J. Truran; W. Hillebrandt

    2001-10-31

    Using the results of recent work in shear instabilities in stratified fluids, we show that the resonant interaction between large-scale flows in the accreted H/He envelope of white dwarf stars and interfacial gravity waves can mix with the star's envelope with the white dwarf's surface material, leading to the enhancement of the envelope's C/O abundance to levels required by extant models for nova outbursts.

  8. SWIFT X-RAY OBSERVATIONS OF CLASSICAL NOVAE. II. THE SUPER SOFT SOURCE SAMPLE

    SciTech Connect (OSTI)

    Schwarz, Greg J.; Ness, Jan-Uwe; Osborne, J. P.; Page, K. L.; Evans, P. A.; Beardmore, A. P.; Walter, Frederick M.; Andrew Helton, L.; Woodward, Charles E.; Bode, Mike; Starrfield, Sumner; Drake, Jeremy J.

    2011-12-01

    The Swift gamma-ray burst satellite is an excellent facility for studying novae. Its rapid response time and sensitive X-ray detector provides an unparalleled opportunity to investigate the previously poorly sampled evolution of novae in the X-ray regime. This paper presents Swift observations of 52 Galactic/Magellanic Cloud novae. We included the X-Ray Telescope (0.3-10 keV) instrument count rates and the UltraViolet and Optical Telescope (1700-8000 A) filter photometry. Also included in the analysis are the publicly available pointed observations of 10 additional novae the X-ray archives. This is the largest X-ray sample of Galactic/Magellanic Cloud novae yet assembled and consists of 26 novae with Super Soft X-ray emission, 19 from Swift observations. The data set shows that the faster novae have an early hard X-ray phase that is usually missing in slower novae. The Super Soft X-ray phase occurs earlier and does not last as long in fast novae compared to slower novae. All the Swift novae with sufficient observations show that novae are highly variable with rapid variability and different periodicities. In the majority of cases, nuclear burning ceases less than three years after the outburst begins. Previous relationships, such as the nuclear burning duration versus t{sub 2} or the expansion velocity of the eject and nuclear burning duration versus the orbital period, are shown to be poorly correlated with the full sample indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst. Finally, we confirm two optical phenomena that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency of X-ray campaigns.

  9. Intial performance from the NOvA surface prototype detector

    SciTech Connect (OSTI)

    Muether, M.; /Fermilab; ,

    2011-09-01

    NOvA, the NuMI Off-Axis {nu}{sub e} Appearance experiment, will study {nu}{sub {mu}} {yields} {nu}{sub e} oscillations characterized by the mixing angle {Theta}{sub 13}. Provided {Theta}{sub 13} is large enough, NOvA may ultimately determine the ordering of the neutrino masses and measure CP violation in neutrino oscillations. A complementary pair of detectors will be constructed {approx}14 mrad off beam axis to optimize the energy profile of the neutrinos. This system consists of a surface based 14 kTon liquid scintillator tracking volume located 810 km from the main injector source (NuMI) in Ash River, Minnesota and a smaller underground 222 Ton near detector at the Fermilab. The first neutrino signals at the Ash River Site are expected prior to the 2012 accelerator shutdown. In the meantime, a near detector surface prototype has been completed and neutrinos from two Fermilab sources have been observed using the same highly segmented PVC and liquid scintillator detector system that will be deployed in the full scale experiment. Design and initial performance characteristics of this prototype system are being fed back into the design for the full NOvA program.

  10. Novae as Tevatrons: Prospects for CTA and IceCube

    E-Print Network [OSTI]

    Metzger, Brian D; Vurm, Indrek; Beloborodov, Andrei; Bartos, Imre; Vlasov, Andrey

    2015-01-01

    The discovery of novae as sources of ~GeV gamma-rays highlights the key role of shocks and relativistic particle acceleration in these transient systems. Although there is evidence for a spectral cut-off above energies ~1-100 GeV at particular epochs in some novae, the maximum particle energy achieved in these accelerators has remained an open question. The high densities of the nova ejecta (~10 orders of magnitude larger than in supernova remnants) render the gas far upstream of the shock neutral and shielded from ionizing radiation. The amplification of the magnetic field needed for diffusive shock acceleration requires ionized gas, thus confining the acceleration process to a narrow photo-ionized layer immediately ahead of the shock. Based on the growth rate in this layer of the hybrid non-resonant cosmic ray current-driven instability (considering also ion-neutral damping), we quantify the maximum particle energy, Emax, across the range of shock velocities and upstream densities of interest. We find value...

  11. THE DUSTY NOVA V1065 CENTAURI (NOVA CEN 2007): A SPECTROSCOPIC ANALYSIS OF ABUNDANCES AND DUST PROPERTIES

    SciTech Connect (OSTI)

    Helton, L. Andrew; Woodward, Charles E.; Gehrz, Robert D.; Walter, Frederick M.; Vanlandingham, Karen; Schwarz, Greg J.; Evans, Aneurin; Ness, Jan-Uwe; Geballe, Thomas R.; Greenhouse, Matthew; Krautter, Joachim; Liller, William; Lynch, David K.; Rudy, Richard J.; Shore, Steven N.; Starrfield, Sumner; Truran, Jim

    2010-11-15

    We examine the ejecta evolution of the classical nova V1065 Centauri, constructing a detailed picture of the system based on spectrophotometric observations obtained from 9 to approximately 900 days post-outburst with extensive coverage from optical to mid-infrared wavelengths. We estimate a reddening toward the system of E(B-V) = 0.5 {+-} 0.1, based upon the B - V color and analysis of the Balmer decrement, and derive a distance estimate of 8.7{sup +2.8}{sub -2.1} kpc. The optical spectral evolution is classified as P {sup o}{sub fe} N{sub ne} A{sub o} according to the CTIO Nova Classification system of Williams et al. Photoionization modeling yields absolute abundance values by number, relative to solar of He/H = 1.6 {+-} 0.3, N/H = 144 {+-} 34, O/H = 58 {+-} 18, and Ne/H = 316 {+-} 58 for the ejecta. We derive an ejected gas mass of M{sub g} = (1.6 {+-} 0.2) x 10{sup -4} M{sub sun}. The infrared excess at late epochs in the evolution of the nova arises from dust condensed in the ejecta composed primarily of silicate grains. We estimate a total dust mass, M{sub d} , of order (0.2-3.7) x 10{sup -7} M{sub sun}, inferred from modeling the spectral energy distribution observed with the Spitzer IRS and Gemini-South GNIRS spectrometers. Based on the speed class, neon abundance, and the predominance of silicate dust, we classify V1065 Cen as an ONe-type classical nova.

  12. The dusty nova V1065 centauri (nova cen 2007) : a spectroscopic analysis of abundances and dust properties.

    SciTech Connect (OSTI)

    Helton, L. A.; Woodward, C. E.; Walter, F. M.; Vanlandingham, K.; Schwarz, G. J.; Evans, A.; Ness, J.-U.; Geballe, T. R.; Gehrz, R. D.; Greenhouse, M.; Krautter, J.; Liller, W.; Lynch, D. K.; Rudy, R. J.; Shore, S. N.; Starrfield, S.; Truran, J. (Physics); (Univ. of Minnesota); (Stony Brook Univ.); (West Chester Univ.); (American Astronomical Society); (Keele Univ.); (European Space Astroomy Centre); (Gemini Observatory); (NASA Goddard Space Flight Center); (Landessternwarte-Zebtrum fur Astronomie der Univ.); (Inst. for Nova Studies); (The Aerospace Corp.); (Univ. di Pisa); (Arizona State Univ.); (Univ. of Chicago)

    2010-10-14

    We examine the ejecta evolution of the classical nova V1065 Centauri, constructing a detailed picture of the system based on spectrophotometric observations obtained from 9 to approximately 900 days post-outburst with extensive coverage from optical to mid-infrared wavelengths. We estimate a reddening toward the system of E(B-V) = 0.5 {+-} 0.1, based upon the B-V color and analysis of the Balmer decrement, and derive a distance estimate of 8.7{sub -2.1}{sup +2.8} kpc. The optical spectral evolution is classified as P{sub fe}{sup o} N{sub ne}A{sub 0} according to the CTIO Nova Classification system of Williams et al. Photoionization modeling yields absolute abundance values by number, relative to solar of He/H = 1.6 {+-} 0.3, N/H = 144 {+-} 34, O/H = 58 {+-} 18, and Ne/H = 316 {+-} 58 for the ejecta. We derive an ejected gas mass of M{sub g} = (1.6 {+-} 0.2) x 10{sup -4} M{circle_dot}. The infrared excess at late epochs in the evolution of the nova arises from dust condensed in the ejecta composed primarily of silicate grains. We estimate a total dust mass, Md , of order (0.2-3.7) x 10{sup -7} M{circle_dot}, inferred from modeling the spectral energy distribution observed with the Spitzer IRS and Gemini-South GNIRS spectrometers. Based on the speed class, neon abundance, and the predominance of silicate dust, we classify V1065 Cen as an ONe-type classical nova.

  13. Thermonuclear Runaways on Accreting White Dwarfs: Models of Classical Novae Explosions

    E-Print Network [OSTI]

    Margarita Hernanz; Jordi Jose

    2000-01-11

    The mechanism of classical novae explosions is explained, together with some of their observational properties. The scarce but not null impact of novae in the chemical evolution of the Milky Way is analyzed, as well as their relevance for the radioactivity in the Galaxy. A special emphasis is given to the predicted gamma-ray emission from novae and its relationship with the thermonuclear model itself and its related nucleosynthesis.

  14. Nucleosynthesis in novae: experimental progress in the determination of nuclear reaction rates

    E-Print Network [OSTI]

    Alain Coc

    2008-01-18

    The sources of nuclear uncertainties in nova nucleosynthesis have been identified using hydrodynamical nova models. Experimental efforts have followed and significantly reduced those uncertainties. This is important for the evaluation of nova contribution to galactic chemical evolution, gamma--ray astronomy and possibly presolar grain studies. In particular, estimations of expected gamma-ray fluxes are essential for the planning of observations with existing or future satellites.

  15. IGR J17098-3628: an X-ray Nova discovered by INTEGRAL

    E-Print Network [OSTI]

    S. A. Grebenev; S. V. Molkov; M. G. Revnivtsev; R. A. Sunyaev

    2007-09-14

    We report the discovery with INTEGRAL on March 24, 2005, and follow-up observations of the distant Galactic X-ray nova IGR J17098-3628.

  16. Detecting Neutrinos with the NOvA Detectors (Other) | SciTech...

    Office of Scientific and Technical Information (OSTI)

    PARTICLES AND FIELDS NOVA; NEUTRINO; NEUTRINO DETECTOR; DETECTOR; COSMIC RAY; NEUTRINO INTERACTION Word Cloud More Like This Multimedia File size NAView Multimedia View Multimedia...

  17. 1360 Barrington Street P.O. Box 1000

    E-Print Network [OSTI]

    Hughes, Larry

    Outhouse, Counsel, Nova Scotia Utility and Review Board, 1601 Lower Water Street, 3rd Floor, Halifax, Nova little to help Nova Scotia obtain energy security or reduce its greenhouse gas emissions. In our Privatization Act of 1992, which states that "the Company shall not construct a generating plant that utilizes

  18. CCD Photometry of Dwarf Nova AL Com in Superoutburst

    E-Print Network [OSTI]

    W. Pych; A. Olech

    1995-09-20

    We report a CCD optical photometry of a dwarf nova AL Com in superoutburst. Before superhumps occurred the light curve was highly variable with dominant periods about 41 minutes and 81.5 minutes for different nights. The period of observed superhumps is 82.5 minutes and seems to be stable. The first harmonic of the basic period is also present. We detected a weak signal corresponding to period 78.1 minutes. One of the periods 78.1 or 81.5 is suspected to be a possible signature of orbital motion in the system.

  19. The peculiar dust shell of Nova DZ Cru (2003).

    SciTech Connect (OSTI)

    Evans, A.; Gehrz, R. D.; Woodward, C. E.; Helton, L. A.; Rushton, M. T.; Bode, M. F.; Krautter, J.; Lyke, J.; Lynch, D. K.; Ness, J.-U.; Starrfield, S.; Truran, J. W.; Wagner, R. M.; Physics; Keele Univ.; Univ. of Minnesota; Univ. of Central Lancashire; Liverpool John Moores Univ.; Zentrum fur Astronomie der Univ. Heidelberg; M. W. Keck Observatory; The Aerospace Corp.; European Space Astronomy Centre; Arizona State Univ.; Univ. of Chicago; Large Binocular Telscope Observatory

    2010-01-01

    We present Spitzer Space Telescope observations of the 'peculiar variable' DZ Cru, identified by Rushton et al. as a classical nova. A dust shell, on which are superimposed a number of features, is prominent in the 5-35 {micro}m range some 4 yr after eruption. We suggest that the dust in DZ Cru is primarily hydrogenated amorphous carbon in which aliphatic bands currently predominate and which may become either predominantly aromatic as the dust is photoprocessed by ultraviolet radiation from the stellar remnant or more likely completely destroyed.

  20. HelioNova S L | 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 J APPENDIX E LISTStar2-0057-EA JumpDuimen River PowerHeckert BXT SolarHelioNova S L Jump to:

  1. Cataventos Novas Energias Brasil Ltda | 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 J APPENDIX E LIST OFAMERICA'SHeavy Electricals Ltd BHEL JumpCMNA PowerCataventos Novas Energias

  2. FEI Nova 200 Dual-Beam SEM/FIB

    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 like submitKansasCommunitiesofExtrans - Permeation Measurement2TargetedFEHM (Finite Nova

  3. Better Buildings Network View, October 2014

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

    Peer Exchange Calls Residential Network Online Group Welcomes 100th Member Outlining Data Needs Optimizes Evaluation Efficiency Nova Scotia Releases Mobile App California...

  4. Better Buildings Residential Network Peer Exchange Call Series...

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

    Ecodrain, Inc. Ecova Efficiency Nova Scotia Elevate Energy emPower Central Coast Energy Coordinating Agency of Philadelphia Energy Efficiency Specialists Environmental Design...

  5. Better Buildings Residential Network Multifamily & Low-Income...

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

    County of San Francisco, CA Community Office for Resource Efficiency (Aspen, CO) Davis Energy Group Efficiency Nova Scotia Elevate Energy (Energy Impact Illinois)...

  6. The Class Idea: Politics, Ideology, and Class Formation in the United States and Canada in the Twentieth Century

    E-Print Network [OSTI]

    Eidlin, Barry

    2012-01-01

    and Labrador, Prince Edward Island, Nova Scotia, NewManitoba, New Brunswick, Prince Edward Island, and Quebec.An eighth jurisdiction, Prince Edward Island, adopted first

  7. BULLETIN OF THE UNITED STATES FISH COMMISSION. 125 With reference to the quantity packed in.the maritime provinces an-

    E-Print Network [OSTI]

    that of the previous year by 1,000,000 cans, that of Nova Scotia by 500,000, and Prince Edward Island by 500,000. Cases

  8. Regional Review on Status and Trends in Aquaculture Development in North America: Canada and the United States of America — 2010

    E-Print Network [OSTI]

    Olin, Paul G.; Smith, James; Nabi, Rashed

    2012-01-01

    26 percent), followed by Prince Edward Island (12 percent),and Labrador, Prince Edward Island, Nova Scotia, and Newthe Atlantic province of Prince Edward Island supplies more

  9. The Class Idea: Politics, Ideology, and Class Formation in the United States and Canada in the Twentieth Century

    E-Print Network [OSTI]

    Eidlin, Barry

    2012-01-01

    and Labrador, Prince Edward Island, Nova Scotia, NewNew Brunswick, Prince Edward Island, and Quebec. Prior toAn eighth jurisdiction, Prince Edward Island, adopted first

  10. Title: Platinum Postal Suite Multiple Enhanced Postal Codes (MEP): Canada Data Creator /

    E-Print Network [OSTI]

    Edward Island, Quebec, Saskatchewan, Yukon Keywords (Subject): Boundaries, Postal Codes, Multiple, New Brunswick, Newfoundland and Labrador, Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince

  11. Regional Review on Status and Trends in Aquaculture Development in North America: Canada and the United States of America — 2010

    E-Print Network [OSTI]

    Olin, Paul G.; Smith, James; Nabi, Rashed

    2012-01-01

    followed by Prince Edward Island (12 percent), Figure 4:and Labrador, Prince Edward Island, Nova Scotia, and NewAtlantic province of Prince Edward Island supplies more than

  12. Metadata Template (Vector and Images) Title: DMTI Census Geography Files 1996

    E-Print Network [OSTI]

    Edward Island, Quebec, Saskatchewan, Yukon Keywords (Subject): Census; Boundaries Restrictions: Data, New Brunswick, Newfoundland and Labrador, Northwest Territories, Nova Scotia, Nunavut, Ontario, Prince

  13. V723 Cas: A dying nova or a new-born SSS? 1 V723 Cas: A dying nova or a new-born SSS?

    E-Print Network [OSTI]

    Ness, Jan-Uwe

    V723 Cas: A dying nova or a new-born SSS? 1 V723 Cas: A dying nova or a new-born SSS? J.-U. Ness, S-rays with Swift and found a clear detection (Ness et al. 2006; 8). There are two possible ex- planations why V723). It can be seen that we have enough sig- #12;2 J.-U. Ness, S.

  14. Submitted to ApJ Letters, June 29, 2005 Are Presolar Silicon Carbide Grains from Novae Actually from Supernovae?

    E-Print Network [OSTI]

    Nittler, Larry R.

    of nucleosynthesis in ONe novae, thermonuclear runaways that occur on O- and Ne-rich white dwarfs in close binary

  15. Swift X-ray and UV monitoring of the Classical Nova V458 Vul (Nova Vul 2007)

    E-Print Network [OSTI]

    Ness, J -U; Beardmore, A P; Boyd, D; Bode, M F; Brady, S; Evans, P A; Gänsicke, B T; Kitamoto, S; Knigge, C; Miller, I; Osborne, J P; Page, K L; Rodríguez-Gil, P; Schwarz, G; Staels, B; Steeghs, D; Takei, D; Tsujimoto, M; Wesson, R; Zijlstra, A

    2009-01-01

    We describe the highly variable X-ray and UV emission of V458 Vul (Nova Vul 2007), observed by Swift between 1 and 422 days after outburst. Initially bright only in the UV, V458 Vul became a variable hard X-ray source due to optically thin thermal emission at kT=0.64 keV with an X-ray band unabsorbed luminosity of 2.3x10^{34} erg s^{-1} during days 71-140. The X-ray spectrum at this time requires a low Fe abundance (0.2^{+0.3}_{-0.1} solar), consistent with a Suzaku measurement around the same time. On day 315 we find a new X-ray spectral component which can be described by a blackbody with temperature of kT=23^{+9}_{-5} eV, while the previous hard X-ray component has declined by a factor of 3.8. The spectrum of this soft X-ray component resembles those typically seen in the class of supersoft sources (SSS) which suggests that the nova ejecta were starting to clear and/or that the WD photosphere is shrinking to the point at which its thermal emission reaches into the X-ray band. We find a high degree of varia...

  16. NOVA-NREL Optimal Vehicle Acquisition Analysis (Brochure)

    SciTech Connect (OSTI)

    Blakley, H.

    2011-03-01

    Federal fleet managers face unique challenges in accomplishing their mission - meeting agency transportation needs while complying with Federal goals and mandates. Included in these challenges are a variety of statutory requirements, executive orders, and internal goals and objectives that typically focus on petroleum consumption and greenhouse gas (GHG) emissions reductions, alternative fuel vehicle (AFV) acquisitions, and alternative fuel use increases. Given the large number of mandates affecting Federal fleets and the challenges faced by all fleet managers in executing day-to-day operations, a primary challenge for agencies and other organizations is ensuring that they are as efficient as possible in using constrained fleet budgets. An NREL Optimal Vehicle Acquisition (NOVA) analysis makes use of a mathematical model with a variety of fleet-related data to create an optimal vehicle acquisition strategy for a given goal, such as petroleum or GHG reduction. The analysis can helps fleets develop a vehicle acquisition strategy that maximizes petroleum and greenhouse gas reductions.

  17. NOvA (Fermilab E929) Official Plots and Figures

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    The NOvA collaboration, consisting of 180 researchers across 28 institutions and managed by the Fermi National Accelerator Laboratory (FNAL), is developing instruments for a neutrino-focused experiment that will attempt to answer three fundamental questions in neutrino physics: 1) Can we observe the oscillation of muon neutrinos to electron neutrinos; 2) What is the ordering of the neutrino masses; and 3) What is the symmetry between matter and antimatter? The collaboration makes various data plots and figures available. These are grouped under five headings, with brief descriptions included for each individual figure: Neutrino Spectra, Detector Overview, Theta12 Mass Hierarchy CP phase, Theta 23 Delta Msqr23, and NuSterile.

  18. Measurement of ICF fuel ion temperature on Nova

    SciTech Connect (OSTI)

    Harris, D.B.; Chrien, R.E.

    1994-02-01

    A new diagnostic for measuring the average fuel ion temperature in inertial confinement fusion (ICF) targets at the time of peak burn has been constructed by Los Alamos and installed on the Nova Laser System at Lawrence Livermore National Laboratory. This ion-temperature diagnostic measures the time-of-flight of fusion neutrons and determines the thermonuclear-reaction-weighted ion temperature through the time-of-arrival distribution. Preliminary experiments have been designed and performed to test the diagnostic. These tests measured the ion temperature of targets designed to have varying temperatures and yields. Additionally, an experiment has been designed to examine the cause of the increase in yield degradation (compared to clean 1-D calculations) as the capsule convergence is increased. Understanding the cause of yield degradation in high convergence implosions is necessary to increase the confidence of the target performance for the next generation National Ignition Facility planned by the US ICF Program.

  19. The {sup 30}P(p, ?){sup 31}S reaction in classical novae: progress and prospects

    SciTech Connect (OSTI)

    Wrede, C., E-mail: wrede@nscl.msu.edu [Department of Physics and Astronomy and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824 (United States)

    2014-04-15

    The unknown thermonuclear rate of the {sup 30}P(p, ?){sup 31}S reaction at classical-nova temperatures currently prohibits the accurate modeling of nova nucleosynthesis in the A ? 30 region. This is hindering the calibration of nova thermometers based on observed O/S, S/Al, O/P, and P/Al abundance ratios in nova ejecta, the calibration of a meter to probe mixing at the core-envelope interface in novae based on the observed Si/H abundance ratio, and the identification of candidate pre-solar nova grains found in primitive meteorites based on laboratory measurements of their {sup 30}Si/{sup 28}Si isotopic ratios. Each of these diagnostics could address key questions in our understanding of classical novae if the {sup 30}P(p, ?){sup 31}S rate were known. We review progress on the determination of the {sup 30}P(p, ?){sup 31}S rate leading to a critical assessment of current interpretations of published data and prospects for future work.

  20. Observations and Analysis of the GK Persei Nova Shell and its "Jet-like" Feature

    E-Print Network [OSTI]

    Harvey, E; Boumis, P; Akras, S

    2016-01-01

    GK Persei (1901, the 'Firework Nebula') is an old but bright nova remnant that offers a chance to probe the physics and kinematics of nova shells. The kinematics in new and archival longslit optical echelle spectra were analysed using the shape software. New imaging from the Aristarchos telescope continues to track the proper motion, extinction and structural evolution of the knots, which have been observed intermittently over several decades. We present for the first time, kinematical constraints on a large faint 'jet' feature, that was previously detected beyond the shell boundary. These observational constraints allow for the generation of models for individual knots, interactions within knot complexes, and the 'jet' feature. Put together, and taking into account dwarf-nova accelerated winds emanating from the central source, these data and models give a deeper insight into the GK Per nova remnant as a whole.

  1. Fermilab | Newsroom | Press Releases | August 7, 2015: NOvA Images

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

    Fermilab Med Res | Hi Res A view across the top of the NOvA far detector in Ash River, Minnesota. Electronics that make up part of the data acquisition system are...

  2. Early optical spectra of nova V1369 Cen show presence of Lithium

    E-Print Network [OSTI]

    Izzo, L; Mason, E; Matteucci, F; Romano, D; Pasquini, L; Vanzi, L; Jordan, A; Fernandez, J M; Bluhm, P; Brahm, R; Espinoza, N; Williams, R

    2015-01-01

    We present early high resolution spectroscopic observations of the nova V1369 Cen. We have detected an absorption feature at 6695.6 \\AA\\, that we have identified as blue--shifted $^7$Li I $\\lambda$6708 \\AA. The absorption line, moving at -550 km/s, was observed in five high-resolution spectra of the nova obtained at different epochs. On the basis of the intensity of this absorption line we infer that a single nova outburst can inject in the Galaxy $M_{Li} =$ 0.3 - 4.8 $\\times 10^{-10}$ M$_{\\odot}$. Given the current estimates of Galactic nova rate, this amount is sufficient to explain the puzzling origin of the overabundance of Lithium observed in young star populations.

  3. Pulsed power supply for Nova Upgrade. Final report, August 1, 1991 to March 31, 1992

    SciTech Connect (OSTI)

    Bacon, J.L.; Kajs, J.P.; Walls, A.; Weldon, W.F.; Zowarka, R.C.

    1992-12-31

    This report describes work carried out at the Center for Electromechanics at The University of Texas at Austin (CEM-UT). A baseline design of the Nova Upgrade has been completed by Lawrence Livermore National Laboratory. The Nova Upgrade is an 18 beamline Nd: glass laser design utilizing fully relayed 4x4 30 cm aperture segmented optical components. The laser thus consists of 288 independent beamlets nominally producing 1.5 to 2.0 MJ of 0.35 {mu}m light in a 3 to 5 ns pulse. The laser design is extremely flexible and will allow a wide range of pulses to irradiate ICF targets. This facility will demonstrate ignition/gain and the scientific feasibility of ICF for energy and defense applications. The pulsed power requirements for the Nova Upgrade are given. CEM-UT was contracted to study and develop a design for a homopolar generator/inductor (HPG/inductor) opening switch system which would satisfy the pulsed power supply requirements of the Nova Upgrade. The Nd:glass laser amplifiers used in the Nova Upgrade will be powered by light from xenon flashlamps. The pulsed power supply for the Nova Upgrade powers the xenon flashlamps. This design and study was for a power supply to drive flashlamps.

  4. Binary orbits as the driver of gamma-ray emission and mass ejection in classical novae

    E-Print Network [OSTI]

    Chomiuk, Laura; Yang, Jun; O'Brien, T J; Paragi, Zsolt; Mioduszewski, Amy J; Beswick, R J; Cheung, C C; Mukai, Koji; Nelson, Thomas; Ribeiro, Valerio A R M; Rupen, Michael P; Sokoloski, J L; Weston, Jennifer; Zheng, Yong; Bode, Michael F; Eyres, Stewart; Roy, Nirupam; Taylor, Gregory B

    2014-01-01

    Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems. Novae typically expel ~10^(-4) solar masses of material at velocities exceeding 1,000 kilometres per second. However, the mechanism of mass ejection in novae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy, prolonged optically thick winds, or binary interaction with the nova envelope. Classical novae are now routinely detected in gigaelectronvolt gamma-ray wavelengths, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the gamma-ray-emitting nova V959 Mon. We find that its ejecta were shaped by the motion of the binary system: some gas was expelled rapidly along the poles as a wind from the white dwarf, while denser material drifted out along the equatorial plane, propelled by orbital motion. At the interface ...

  5. A tomographic study of the classical nova RR Pic

    E-Print Network [OSTI]

    Fabiola M. A. Ribeiro; Marcos P. Diaz

    2005-10-03

    We present the results of spectrophotometric observations of the old nova RR Pic performed in two spectral ranges, one centered in the Ha line and other covering Hb and Hg spectral lines. From the Hb radial velocity study we found a primary radial semi-amplitude of K1 = 37(1) km/s and a systemic velocity of g = 1.8(2) km/s. With this new values a mass diagram is constructed, constraining the possible mass intervals for the system. The possible orbital inclination range was restricted using the fact that RR Pic presents shallow eclipses. A secondary mass range below the limit of a main sequence star filling its Roche lobe indicate an evolved companion. We also calculated the Ha, Hb, Hg, HeI 6678 and HeII 4686 Doppler tomograms. The most conspicuous differences are found between the HeI and HeII tomograms, the former has a ring shape, while the second is filled at low velocities, suggesting that the low velocity emission is not coming from the accretion disk. Radial emissivity profiles for these lines were also derived.

  6. SWIFT X-RAY AND ULTRAVIOLET MONITORING OF THE CLASSICAL NOVA V458 VUL (NOVA VUL 2007)

    SciTech Connect (OSTI)

    Ness, J.-U. [European Space Astronomy Centre, P.O. Box 78, 28691 Villanueva de la Canada, Madrid (Spain); Drake, J. J. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Beardmore, A. P.; Evans, P. A.; Osborne, J. P.; Page, K. L. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Boyd, D. [BAA VSS, 5 Silver Lane, West Challow, Wantage, OX12 9TX (United Kingdom); Bode, M. F. [Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD (United Kingdom); Brady, S. [AAVSO, 5 Melba Drive, Hudson, NH 03051 (United States); Gaensicke, B. T.; Steeghs, D. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Kitamoto, S.; Takei, D. [Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo 171-8501 (Japan); Knigge, C. [School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ (United Kingdom); Miller, I. [BAA VSS, Furzehill House, Ilston, Swansea SA2 7LE (United Kingdom); Rodriguez-Gil, P. [Isaac Newton Group, PO Ap. de Correos 321, 38700 Sta. Cruz de la Palma (Spain); Schwarz, G. [Department of Geology and Astronomy, West Chester University, West Chester, PA 19383 (United States); Staels, B. [CBA Flanders, Alan Guth Observatory, Koningshofbaan 51, Hofstade, Aalst (Belgium); Tsujimoto, M. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States); Wesson, R. [Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT (United Kingdom)], E-mail: juness@sciops.esa.int (and others)

    2009-05-15

    We describe the highly variable X-ray and UV emission of V458 Vul (Nova Vul 2007), observed by Swift between 1 and 422 days after outburst. Initially bright only in the UV, V458 Vul became a variable hard X-ray source due to optically thin thermal emission at kT = 0.64 keV with an X-ray band unabsorbed luminosity of 2.3 x 10{sup 34} erg s{sup -1} during days 71-140. The X-ray spectrum at this time requires a low Fe abundance (0.2{sup +0.3} {sub -0.1} solar), consistent with a Suzaku measurement around the same time. On day 315 we find a new X-ray spectral component which can be described by a blackbody with temperature of kT = 23{sup +9} {sub -5} eV, while the previous hard X-ray component has declined by a factor of 3.8. The spectrum of this soft X-ray component resembles those typically seen in the class of supersoft sources (SSS) which suggests that the nova ejecta were starting to clear and/or that the white dwarf photosphere is shrinking to the point at which its thermal emission reaches into the X-ray band. We find a high degree of variability in the soft component with a flare rising by an order of magnitude in count rate in 0.2 days. In the following observations on days 342.4-383.6, the soft component was not seen, only to emerge again on day 397. The hard component continued to evolve, and we found an anticorrelation between the hard X-ray emission and the UV emission, yielding a Spearman rank probability of 97%. After day 397, the hard component was still present, was variable, and continued to fade at an extremely slow rate but could not be analyzed owing to pile-up contamination from the bright SSS component.

  7. Department

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  8. Department

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  9. Some electric myths Larry Hughes

    E-Print Network [OSTI]

    Hughes, Larry

    in residential electricity demand (133 GWh). If these trends continue into the fourth quarter, Nova Scotia Power of the rise in residential electricity demand is the result of the increased use of electricity for space of coal and Nova Scotia's demand for electricity, both of which are based, in part, upon the arguments

  10. Response to Electricity Review Report Draft 18 February 2015 Larry Hughes, PhD

    E-Print Network [OSTI]

    Hughes, Larry

    to the retail market. One of the first outcomes of the public consultations was the Electricity Review Report and organizations have successfully pressured both the provincial government and Nova Scotia Power to address some thermal-coal based electricity supplier, Nova Scotia Power, although still heavily reliant on coal

  11. Isotopic 32S/33S ratio as a diagnostic of presolar grains from novae

    E-Print Network [OSTI]

    A. Parikh; K. Wimmer; T. Faestermann; R. Hertenberger; J. Jose; H. -F. Wirth; C. Hinke; R. Krucken; D. Seiler; K. Steiger; K. Straub

    2014-09-01

    Measurements of sulphur isotopes in presolar grains can help to identify the astrophysical sites in which these grains were formed. A more precise thermonuclear rate of the 33S(p,gamma)34Cl reaction is required, however, to assess the diagnostic ability of sulphur isotopic ratios. We have studied the 33S(3He,d)34Cl proton-transfer reaction at 25 MeV using a high-resolution quadrupole-dipole-dipole-dipole magnetic spectrograph. Deuteron spectra were measured at ten scattering angles between 10 and 55 degrees. Twenty-four levels in 34Cl over Ex = 4.6 - 5.9 MeV were observed, including three levels for the first time. Proton spectroscopic factors were extracted for the first time for levels above the 33S+p threshold, spanning the energy range required for calculations of the thermonuclear 33S(p,gamma)34Cl rate in classical nova explosions. We have determined a new 33S(p,gamma)34Cl rate using a Monte Carlo method and have performed new hydrodynamic nova simulations to determine the impact on nova nucleosynthesis of remaining nuclear physics uncertainties in the reaction rate. We find that these uncertainties lead to a factor of less than 5 variation in the 33S(p,gamma)34Cl rate over typical nova peak temperatures, and variation in the ejected nova yields of S--Ca isotopes by less than 20%. In particular, the predicted 32S/33S ratio is 110 - 130 for the nova model considered, compared to 110 - 440 with previous rate uncertainties. As recent type II supernova models predict ratios of 130 - 200, the 32S/33S ratio may be used to distinguish between grains of nova and supernova origin.

  12. The Turn-off of Classical Novae Observed Through X-rays: Models versus ROSAT Observations of V1974 Cyg

    E-Print Network [OSTI]

    Gloria Sala; Margarita Hernanz

    2004-10-05

    Detection of X-ray emission from classical novae in their post-outburst stages provides crucial information about the nova phenomenon. The soft X-ray emission gives a direct insight into the remaining hot nuclear burning shell. A numerical model for steady H-burning white dwarf envelopes has been developed to study the post-outburst phases of classical novae. Properties of the X-ray emission of the post-nova white dwarf are obtained, and the results are compared to ROSAT observations of V1974 Cyg.

  13. Outburst-related period changes of recurrent nova CI aquilae

    SciTech Connect (OSTI)

    Wilson, R. E.; Honeycutt, R. K., E-mail: honey@astro.indiana.edu, E-mail: rewilson@ufl.edu [Astronomy Department, Indiana University, Swain Hall West, Bloomington, IN 47405 (United States)

    2014-11-01

    Pre-outburst and post-outburst light curves and post-outburst eclipse timings are analyzed to measure any period (P) change related to nova CI Aql's outburst of early 2000 and a mean post-outburst dP/dt, which then lead to estimates of the accreting component's rate of mass (M) change and its overall outburst-related change of mass over roughly a decade of observations. We apply a recently developed procedure for unified analysis of three timing-related data types (light curves, radial velocities, and eclipse timings), although with only light curves and timings in this case. Fits to the data are reasonably good without need for a disk in the light-curve model, although the disk certainly exists and has an important role in our post-outburst mass flow computations. Initial experiments showed that, although there seems to be an accretion hot spot, it has essentially no effect on derived outburst-related ?P or on post-outburst dP/dt. Use of atomic time (HJED) in place of HJD also has essentially nil effect on ?P and dP/dt. We find ?P consistently negative in various types of solutions, although at best only marginally significant statistically in any one experiment. Pre-outburst HJD {sub 0} and P results are given, as are post-outburst HJD {sub 0}, P, and dP/dt, with light curves and eclipse times as joint input, and also with only eclipse time input. Post-outburst dP/dt is negative at about 2.4?. Explicit formulae for mass transfer rates and epoch-to-epoch mass change are developed and applied. A known offset in the magnitude zero point for 1991-1994 is corrected.

  14. Nuclear ashes and outflow in the eruptive star Nova Vul 1670

    E-Print Network [OSTI]

    Kaminski, Tomasz; Tylenda, Romuald; Hajduk, Marcin; Patel, Nimesh A; Kraus, Alexander

    2015-01-01

    CK Vulpeculae was observed in outburst in 1670-16721, but no counterpart was seen until 1982, when a bipolar nebula was found at its location. Historically, CK Vul has been considered to be a nova (Nova Vul 1670), but a similarity to 'red transients', which are more luminous than classical nova and thought to be the result of stellar collisions, has re-opened the question of CK Vul's status. Red transients cool to resemble late M-type stars, surrounded by circumstellar material rich in molecules and dust. No stellar source has been seen in CK Vul, though a radio continuum source was identified at the expansion centre of the nebula. Here we report CK Vul is surrounded by chemically rich molecular gas with peculiar isotopic ratios, as well as dust. The chemical composition cannot be reconciled with a nova or indeed any other known explosion. In addition, the mass of the surrounding gas is too high for a nova, though the conversion from observations of CO to a total mass is uncertain. We conclude that CK Vul is ...

  15. X-ray Study of Rekindled Accretion in the Classical Nova V2491 Cygni

    E-Print Network [OSTI]

    Takei, D; Tsujimoto, M; Kitamoto, S; Drake, J J; Osborne, J P; Takahashi, H; Kinugasa, K

    2011-01-01

    We conducted an X-ray spectroscopic study of the classical nova V2491 Cygni using our target-of-opportunity observation data with the Suzaku and XMM-Newton satellites as well as archived data with the Swift satellite. Medium-resolution (R~10-50) spectra were obtained using the X-ray CCD spectrometers at several post-nova epochs on days 9, 29, 40, 50, and 60-150 in addition to a pre-nova interval between days -322 and -100 all relative to the time when the classical nova was spotted. We found remarkable changes in the time series of the spectra: (a) In the pre-nova phase and on day 9, the 6.7 keV emission line from Fe XXV was significantly detected. (b) On day 29, no such emission line was found. (c) On day 40, the 6.7 keV emission line emerged again. (d) On days 50 and 60-150, three emission lines at 6.4, 6.7, and 7.0 keV respectively from quasi-neutral Fe, Fe XXV, and Fe XXVI were found. Statistically significant changes of the Fe K line intensities were confirmed between day 29 and 50. Based on these phenom...

  16. The Effects of Thermonuclear Reaction Rate Variations on Nova Nucleosynthesis: A Sensitivity Study

    E-Print Network [OSTI]

    Christian Iliadis; Art Champagne; Jordi Jose; Sumner Starrfield; Paul Tupper

    2002-06-03

    We investigate the effects of thermonuclear reaction rate uncertainties on nova nucleosynthesis. One-zone nucleosynthesis calculations have been performed by adopting temperature-density-time profiles of the hottest hydrogen-burning zone (i.e., the region in which most of the nucleosynthesis takes place). We obtain our profiles from 7 different, recently published, hydrodynamic nova simulations covering peak temperatures in the range from Tpeak=0.145-0.418 GK. For each of these profiles, we individually varied the rates of 175 reactions within their associated errors and analyzed the resulting abundance changes of 142 isotopes in the mass range below A=40. In total, we performed 7350 nuclear reaction network calculations. We use the most recent thermonuclear reaction rate evaluations for the mass ranges A=1-20 and A=20-40. For the theoretical astrophysicist, our results indicate the extent to which nova nucleosynthesis calculations depend on presently uncertain nuclear physics input, while for the experimental nuclear physicist our results represent at least a qualitative guide for future measurements at stable and radioactive ion beam facilities. We find that present reaction rate estimates are reliable for predictions of Li, Be, C and N abundances in nova nucleosynthesis. However, rate uncertainties of several reactions have to be reduced significantly in order to predict more reliable O, F, Ne, Na, Mg, Al, Si, S, Cl and Ar abundances. Results are presented in tabular form for each adopted nova simulation.

  17. Department

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  18. Department

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  19. Department

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  20. Department

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  1. Department

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  2. Department

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  3. Department

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  4. Department

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  6. Department

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  7. Department

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  8. Department

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  9. Department

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  10. Department

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  11. Department

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  12. Department

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  13. Department

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  14. Department

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  15. Department

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  16. Department

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  17. Department

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  18. Department

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  19. Department

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  20. Department

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  1. Department

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  2. Department

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  3. Department

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  4. Department

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  5. Construction of AC Motor Controllers for NOvA Experiment Upgrades

    SciTech Connect (OSTI)

    Cooley, Patrick; ,

    2011-08-04

    I have been constructing Alternating Current (AC) motor controllers for manipulation of particle beam detectors. The capability and reliability of these motor controllers are essential to the Laboratory's mission of accurate analysis of the particle beam's position. The device is moved in and out of the beam's path by the motor controller followed by the Neutrinos at the Main Injector Off-Axis {nu}{sub e} Appearance (NOvA) Experiment further down the beam pipe. In total, I built and tested ten ac motor controllers for new beam operations in the NOvA experiment. These units will prove to be durable and provide extremely accurate beam placement for NOvA Experiment far into the future.

  6. Using near detector(s) to predict the far detector events in NOvA experiment

    SciTech Connect (OSTI)

    Djurcic, Zelimir; /Argonne

    2011-01-01

    The NOvA experiment is designed to search for a non-vanishing mixing angle {theta}{sub 13} with unprecedented sensitivity and has the potential to resolve the neutrino mass hierarchy and constrain CP-violation phase. NOvA will use two functionally identical detectors at near and far locations to eliminate sensitivity to modeling of neutrino flux and cross-sections. The near detector will measure neutrino rate to constrain backgrounds expected in the far detector which will search for appearance of electron neutrinos and/or anti-neutrinos using Fermilab NuMI neutrino beam. This report describes initial thoughts on how the available beams and detectors may be used to reach the NOvA goals.

  7. The Impact of Nuclear Reaction Rate Uncertainties on Evolutionary Studies of the Nova Outburst

    E-Print Network [OSTI]

    W. Raphael Hix; Michael S. Smith; Anthony Mezzacappa; Sumner Starrfield; Donald L. Smith

    2000-01-27

    The observable consequences of a nova outburst depend sensitively on the details of the thermonuclear runaway which initiates the outburst. One of the more important sources of uncertainty is the nuclear reaction data used as input for the evolutionary calculations. A recent paper by Starrfield, Truran, Wiescher, & Sparks (1998) has demonstrated that changes in the reaction rate library used within a nova simulation have significant effects, not just on the production of individual isotopes (which can change by an order of magnitude), but on global observables such as the peak luminosity and the amount of mass ejected. We present preliminary results of systematic analyses of the impact of reaction rate uncertainties on nova nucleosynthesis.

  8. Modeling CHANDRA Low Energy Transmission Grating Spectrometer Observations of Classical Novae with PHOENIX

    E-Print Network [OSTI]

    Alexander Petz; Peter H. Hauschildt; Jan-Uwe Ness; Sumner Starrfield

    2005-01-05

    We use the PHOENIX code package to model the X-ray spectrum of Nova V4743 Sagittarii observed with the LETGS onboard the Chandra satellite on 19 March 2003. To analyze nova atmospheres and related systems with an underlying nuclear burning envelope at X-ray wavelengths, it was necessary to update the code with new microphysics. We demonstrate that the X-ray emission is dominated by thermal bremsstrahlung and that the hard X-rays are dominated by Fe and N absorption. Preliminary models are calculated assuming solar abundances. It is shown that the models can be used to determine element abundances in the nova ejecta by increasing the absorption in the shell.

  9. Newly arising problems in the research of SU UMa-type dwarf novae from VSNET collaborations

    E-Print Network [OSTI]

    D. Nogami

    2006-05-10

    Our research on variable objects based on the VSNET collaborations has achieved much progress in understanding the nature of many kinds of phenomena. Many problems have appeared, instead. Among them, we here review three newly arising problems in the research of SU UMa-type dwarf novae: 1) how do EI Psc and V485 Cen evolve as a cataclysmic variable?, 2) is the early superhump a particular phenomenon for WZ Sge-type dwarf novae?, and 3) what parameters determine variations of the superhump period?

  10. jhchang@nova.snu.ac.kr {btzhang,ytkim}@cse.snu.ac.kr Helmholtz machine

    E-Print Network [OSTI]

    jhchang@nova.snu.ac.kr {btzhang,ytkim}@cse.snu.ac.kr Helmholtz machine . Helmholtz machine , . Helmholtz machine . , . (information gain) , Naïve Bayes . 1. (text categorization) . , . k- , Naïve Bayes, , support vector machine, PCA . , . . , . MCMC (Markov Chain Monte Carlo), Variational inference . Helmholtz

  11. Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)

    E-Print Network [OSTI]

    Weston, Jennifer H S; Chomiuk, Laura; Linford, Justin D; Nelson, Thomas; Mukai, Koji; Finzell, Tom; Mioduszewski, Amy; Rupen, Michael P; Walter, Frederick M

    2015-01-01

    Since the Fermi discovery of $\\gamma$-rays from novae, one of the biggest questions in the field has been how novae generate such high-energy emission. Shocks must be a fundamental ingredient. Six months of radio observations of the 2012 nova V5589 Sgr with the VLA and 15 weeks of X-ray observations with Swift/XRT show that the radio emission consisted of: 1) a shock-powered, non-thermal flare; and 2) weak thermal emission from $10^{-5}$ M$_\\odot$ of freely expanding, photoionized ejecta. Absorption features in the optical spectrum and the peak optical brightness suggest that V5589 Sgr lies at 4 kpc (3.2-4.6 kpc). The shock-powered flare was the dominant component in the radio light curve at low frequencies before day 100. The spectral evolution of the flare, its high radio brightness temperature, the presence of unusually hard ($kT_x > 33$ keV) X-rays, and the ratio of radio to X-ray flux near the peak of the flare all support the conclusions that the flare is shock-powered and non-thermal. Unlike other nova...

  12. Solar Sails: una nova manera de navegar per l'espai A. Farres1

    E-Print Network [OSTI]

    Rovira, Carles

    Solar Sails: una nova manera de navegar per l'espai (SIMBa) A. Farr´es1 & `A. Jorba2 1 Institut de Dynamics Station Keeping Surfing + realistic model Conclusions 1 Background on Solar Sails 2 Some comments) Solar Sails SIMBa 2 / 62 #12;Background Dynamics Station Keeping Surfing + realistic model Conclusions

  13. Concurrent Formation of Carbon and Silicate Dust in Nova V1280 Sco

    E-Print Network [OSTI]

    Sakon, Itsuki; Onaka, Takashi; Nozawa, Takaya; Kimura, Yuki; Fujiyoshi, Takuya; Shimonishi, Takashi; Usui, Fumihiko; Takahashi, Hidenori; Ohsawa, Ryou; Arai, Akira; Uemura, Makoto; Nagayama, Takahiro; Koo, Bon-Chul; Kozasa, Takashi

    2015-01-01

    We present infrared multi-epoch observations of the dust forming nova V1280 Sco over $\\sim$2000 days from the outburst. The temporal evolution of the infrared spectral energy distributions at 1272, 1616 and 1947 days can be explained by the emissions produced by amorphous carbon dust of mass (6.6--8.7)$\\times$10$^{-8}$M$_{\\odot}$ with a representative grain size of 0.01$~\\mu$m and astronomical silicate dust of mass (3.4--4.3)$\\times$10$^{-7}$M$_{\\odot}$ with a representative grain size of 0.3--0.5$~\\mu$m. Both of these dust species travel farther away from the white dwarf without an apparent mass evolution throughout those later epochs. The dust formation scenario around V1280 Sco suggested from our analyses is that the amorphous carbon dust is formed in the nova ejecta followed by the formation of silicate dust in the expanding nova ejecta or as a result of the interaction between the nova wind and the circumstellar medium.

  14. The mass of the white dwarf in the old nova BT Mon

    E-Print Network [OSTI]

    D. A. Smith; V. S. Dhillon; T. R. Marsh

    1997-09-22

    We present spectrophotometry of the eclipsing old nova BT Mon (Nova Mon 1939). By detecting weak absorption features from the secondary star, we find its radial velocity semi-amplitude to be K_R = 205+/-5 km/s and its rotational velocity to be vsin i = 138+/-5 km/s. We also measure the radial velocity semi-amplitude of the primary star to be K_R = 170+/-10 km/s. From these parameters we obtain a mass of 1.04+/-0.06 M_sun for the white dwarf primary star and a mass of 0.87+/-0.06 M_sun for the G8V secondary star. The inclination of the system is found to be 82.2+/-3.2 deg and we estimate that the system lies at a distance of 1700+/-300pc. The high mass of the white dwarf and our finding that BT Mon was probably a fast nova together constitute a new piece of evidence in favour of the thermonuclear runaway model of classical nova outbursts. The emission lines are single peaked throughout the orbital cycle, showing absorption around phase 0.5, high velocity S-wave components and large phase offsets in their radial velocity curves. In each of these respects, BT Mon is similar to the SW Sex stars. We also find quasi-periodic flaring in the trailed spectra, which makes BT Mon a candidate intermediate polar.

  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. Underground study of the 17 O(p,? )18F reaction at Gamow energies for classical novae 

    E-Print Network [OSTI]

    Scott, David Andrew

    2014-11-27

    Classical novae are explained as thermonuclear explosions on the surface of white dwarf stars accreting hydrogen-rich material from less evolved companions in binary star systems. These events occur frequently within our ...

  17. Determining the neutrino mass hierarchy and CP violation in NoVA with a second off-axis detector

    SciTech Connect (OSTI)

    Mena, Olga; /Fermilab; Palomares-Ruiz, Sergio; /Vanderbilt U.; Pascoli, Silvia; /CERN /Durham U., IPPP

    2005-10-01

    We consider a Super-NOVA-like experimental configuration based on the use of two detectors in a long-baseline experiment as NOVA. We take the far detector as in the present NOVA proposal and add a second detector at a shorter baseline. The location of the second off-axis detector is chosen such that the ratio L/E is the same for both detectors, being L the baseline and E the neutrino energy. We consider liquid argon and water- Cerenkov techniques for the second off-axis detector and study, for different experimental setups, the detector mass required for the determination of the neutrino mass hierarchy, for different values of {theta}{sub 13}. We also study the capabilities of such an experimental setup for determining CP-violation in the neutrino sector. Our results show that by adding a second off-axis detector a remarkable enhancement on the capabilities of the current NOVA experiment could be achieved.

  18. High Energy Neutrinos from Novae in Symbiotic Binaries: The Case of V407 Cygni

    E-Print Network [OSTI]

    Soebur Razzaque; Pierre Jean; Olga Mena

    2010-12-07

    Detection of high-energy (~> 100 MeV) gamma rays by the Fermi Large Area Telescope (LAT) from a nova in the symbiotic binary system V407 Cygni has opened possibility of high-energy neutrino detection from this type of sources. Thermonuclear explosion on the white dwarf surface sets off a nova shell in motion that expands and slows down in a dense surrounding medium provided by the red giant companion. Particles are accelerated in the shocks of the shell, and interact with surrounding medium to produce observed gamma rays. We show that proton-proton interaction, which is most likely responsible for producing gamma rays via neutral pion decay, produces ~> 0.1 GeV neutrinos that can be detected by the current and future experiments at ~> 10 GeV.

  19. ELEMENTAL ABUNDANCES IN THE EJECTA OF OLD CLASSICAL NOVAE FROM LATE-EPOCH SPITZER SPECTRA

    SciTech Connect (OSTI)

    Helton, L. Andrew; Vacca, William D.; Gehrz, Robert D.; Woodward, Charles E.; Shenoy, Dinesh P.; Wagner, R. Mark; Evans, Aneurin; Krautter, Joachim; Schwarz, Greg J.; Starrfield, Sumner

    2012-08-10

    We present Spitzer Space Telescope mid-infrared IRS spectra, supplemented by ground-based optical observations, of the classical novae V1974 Cyg, V382 Vel, and V1494 Aql more than 11, 8, and 4 years after outburst, respectively. The spectra are dominated by forbidden emission from neon and oxygen, though in some cases, there are weak signatures of magnesium, sulfur, and argon. We investigate the geometry and distribution of the late time ejecta by examination of the emission line profiles. Using nebular analysis in the low-density regime, we estimate lower limits on the abundances in these novae. In V1974 Cyg and V382 Vel, our observations confirm the abundance estimates presented by other authors and support the claims that these eruptions occurred on ONe white dwarfs (WDs). We report the first detection of neon emission in V1494 Aql and show that the system most likely contains a CO WD.

  20. NOVA: a nonvariational code for solving MHD stability of axisymmetric toroidal plasmas

    SciTech Connect (OSTI)

    Cheng, C.Z.; Chance, M.S.

    1986-04-01

    A nonvariational approach for determining the ideal MHD stability of axisymmetric toroidal confinement systems is presented. The code (NOVA) employs cubic B-spline finite elements and Fourier expansion in a general flux coordinate (psi, theta, zeta) system. Better accuracy and faster convergence were obtained in comparison with the variational PEST and ERATO codes. The nonvariational approach can be extended to problems having non-Hermitian eigenmode equations where variational energy principles cannot be obtained.

  1. Genetic and environmental factors affecting growth and reproduction characters of Morada Nova sheep in Northeastern Brazil 

    E-Print Network [OSTI]

    Fernandes, Antonio Amaury Oria

    1985-01-01

    sheep was raised at the Fazenda Iracema-Sertao Central Research Unit which belongs to the "Empresa de Pesquisa Agropecuaria do Ceara" (EPACE). The Fazenda Iracema is located at Quixada, Ceara, Brazil situ- Table 3 Summary of the Experimental Morada... collected over a 6-year period (1979-1984) from the Morada Nova sheep flock (Figure 2) maintained by the Experimental Research Unit of the "Empresa de Pesquisa Agropecuaria do Ceara" (EPACE) at the Experimental Iracema Farm, Quixada, Ceara, Brazil...

  2. Superhumps and Repetitive Rebrightenings of the WZ Sge-Type Dwarf Nova, EG Cancri

    E-Print Network [OSTI]

    T. Kato; D. Nogami; K. Matsumoto; H. Baba

    2003-10-15

    We report on time-resolved photometric observations of the WZ Sge-type dwarf nova, EG Cnc (Huruhata's variable, see also http://www.kusastro.kyoto-u.ac.jp/vsnet/DNe/egcnc.html), during its superoutburst in 1996-1997. EG Cnc, after the main superoutburst accompanied with development of superhumps typical of a WZ Sge-type dwarf nova, exhibited a series of six major rebrightenings. During these rebrightenings and the following long fading tail, EG Cnc persistently showed superhumps having a period equal to the superhump period observed during the main superoutburst. The persistent superhumps had a constant superhump flux with respect to the rebrightening phase. These findings suggest the superhumps observed during the rebrightening stage and the fading tail are a "remnant" of usual superhumps, and are not newly triggered by rebrightenings. By comparison with the 1977 outburst of this object and outbursts of other WZ Sge-type dwarf novae, we propose an activity sequence of WZ Sge-type superoutbursts, in which the current outburst of EG Cnc is placed between a single-rebrightening event and distinct outbursts separated by a dip. The post-superoutburst behavior of WZ Sge-type dwarf novae can be understood in the presence of considerable amount of remnant matter behind the cooling front in the outer accretion disk, even after the main superoutburst. We consider the premature quenching of the hot state due to the weak tidal effect under the extreme mass ratio of the WZ Sge-type binary is responsible for the origin of the remnant mass.

  3. Photometry of the dwarf nova AW Sagittae during the 2006 November superoutburst

    E-Print Network [OSTI]

    Jeremy Shears; Roger Pickard; Tom Krajci; Gary Poyner

    2007-05-31

    During 2006 November an outburst of the dwarf nova AW Sge was observed using CCD photometry. This revealed 0.25 magnitude superhumps confirming it to be a superoutburst, possibly only the second confirmed such outburst of this star. The superhumps were observed for 4 days and had a stable period Psh = 0.0745(2)d, a value which is consistent with Psh measured during the 2000 superoutburst.

  4. Nuclear structure of 30S and its implications for nucleosynthesis in classical novae

    E-Print Network [OSTI]

    K. Setoodehnia; A. A. Chen; D. Kahl; T. Komatsubara; J. José; R. Longland; Y. Abe; D. N. Binh; J. Chen; S. Cherubini; J. A. Clark; C. M. Deibel; S. Fukuoka; T. Hashimoto; T. Hayakawa; J. Hendriks; Y. Ishibashi; Y. Ito; S. Kubono; W. N. Lennard; T. Moriguchi; D. Nagae; R. Nishikiori; T. Niwa; A. Ozawa; P. D. Parker; D. Seiler; T. Shizuma; H. Suzuki; C. Wrede; H. Yamaguchi; T. Yuasa

    2012-10-03

    The uncertainty in the 29P(p,gamma)30S reaction rate over the temperature range of 0.1 - 1.3 GK was previously determined to span ~4 orders of magnitude due to the uncertain location of two previously unobserved 3+ and 2+ resonances in the 4.7 - 4.8 MeV excitation region in 30S. Therefore, the abundances of silicon isotopes synthesized in novae, which are relevant for the identification of presolar grains of putative nova origin, were uncertain by a factor of 3. To investigate the level structure of 30S above the proton threshold (4394.9(7) keV), a charged-particle spectroscopy and an in-beam gamma-ray spectroscopy experiments were performed. Differential cross sections of the 32S(p,t)30S reaction were measured at 34.5 MeV. Distorted wave Born approximation calculations were performed to constrain the spin-parity assignments of the observed levels. An energy level scheme was deduced from gamma-gamma coincidence measurements using the 28Si(3He,n-gamma)30S reaction. Spin-parity assignments based on measurements of gamma-ray angular distributions and gamma-gamma directional correlation from oriented nuclei were made for most of the observed levels of 30S. As a result, the resonance energies corresponding to the excited states in 4.5 MeV - 6 MeV region, including the two astrophysically important states predicted previously, are measured with significantly better precision than before. The uncertainty in the rate of the 29P(p,gamma)30S reaction is substantially reduced over the temperature range of interest. Finally, the influence of this rate on the abundance ratios of silicon isotopes synthesized in novae are obtained via 1D hydrodynamic nova simulations.

  5. Non-Thermal Radio Emission from Colliding Flows in Classical Nova V1723 Aql

    E-Print Network [OSTI]

    Weston, Jennifer H S; Metzger, Brian D; Zheng, Yong; Chomiuk, Laura; Krauss, Miriam I; Linford, Justin; Nelson, Thomas; Mioduszewski, Amy; Rupen, Michael P; Finzell, Tom; Mukai, Koji

    2015-01-01

    The importance of shocks in nova explosions has been highlighted by the recent discovery of \\gamma-ray producing novae by Fermi. We use over three years of multi-band radio observations of nova V1723 Aql with the Karl G. Jansky Very Large Array (VLA) to show that shocks between fast and slow flows within the ejecta led to the acceleration of particles and the production of synchrotron radiation. Approximately one month after the start of V1723 Aql's eruption in 2010 September, shocks in the ejecta produced an unexpected radio flare, ultimately resulting in a radio light curve with a multi-peaked structure. More than a year after the start of the eruption, the radio emission became consistent with emanating from an expanding thermal remnant with a mass of $2\\times10^{-4}$ M$_\\odot$ and a temperature of $10^4$ K. However, the brightness temperature of greater than $10^6$ K at low frequencies during the first two months was too high to be due to thermal emission from the small amount of X-ray producing shock-hea...

  6. Recycler Chromaticities and End Shims for NOvA at Fermilab

    SciTech Connect (OSTI)

    Xiao, M.; /Fermilab

    2012-05-01

    In era of NOvA operation, it is planned to slip-stack six on six Booster proton batches in the Recycler ring for a total intensity of 5 x 10{sup 13} protons/cycle. During the slip-stacking, the chromaticities are required to be jumped from (-2,-2) to (-20,-20). However, with the existing 2 families of powered sextupoles in the lattice, the chromaticities can only be adjusted to (-12,-12) from (-2,-2). On the other hand, the presently designed Recycler lattice for Nova replaces the 30 straight section with 8 'D-D half FODO cells'. With the limit of the feasible quad strength, 3 quads in a half-cell were used to obtain the working point under, and the maximum beta-functions in this section cannot be less than 80 m. In this paper, we re-designed the end shims of the permanent magnets in the ring lattice with appropriate quadrupole and sextupole components to meet both chromaticity and tune requirements. We are able to use 2 quads in a half cell in RR30 straight section within feasible quad strength. The maximum beta-functions are also lowered to around 55 m. The dynamic aperture tracking has been done using MAD to simulate the scenario of beam injection into the Recycler ring for Nova.

  7. Thermal radio emission from novae & symbiotics with the Square Kilometre Array

    E-Print Network [OSTI]

    O'Brien, Tim; Chomiuk, Laura; Ribeiro, Valerio; Bode, Michael; Sokoloski, Jennifer; Woudt, Patrick

    2015-01-01

    The thermal radio emission of novae during outburst enables us to derive fundamental quantities such as the ejected mass, kinetic energy, and density profile of the ejecta. Recent observations with newly-upgraded facilities such as the VLA and e-MERLIN are just beginning to reveal the incredibly complex processes of mass ejection in novae (ejections appear to often proceed in multiple phases and over prolonged timescales). Symbiotic stars can also exhibit outbursts, which are sometimes accompanied by the expulsion of material in jets. However, unlike novae, the long-term thermal radio emission of symbiotics originates in the wind of the giant secondary star, which is irradiated by the hot white dwarf. The effect of the white dwarf on the giant's wind is strongly time variable, and the physical mechanism driving these variations remains a mystery (possibilities include accretion instabilities and time-variable nuclear burning on the white dwarf's surface). The exquisite sensitivity of SKA1 will enable us to su...

  8. X-Ray Emitting Blast Wave from the Recurrent Nova RS Ophiuchi

    E-Print Network [OSTI]

    J. L. Sokoloski; G. J. M. Luna; K. Mukai; Scott J. Kenyon

    2006-05-30

    Stellar explosions such as novae and supernovae produce most of the heavy elements in the Universe. Although the onset of novae from runaway thermonuclear fusion reactions on the surface of a white dwarf in a binary star system is understood[1], the structure, dynamics, and mass of the ejecta are not well known. In rare cases, the white dwarf is embedded in the wind nebula of a red-giant companion; the explosion products plow through the nebula and produce X-ray emission. Early this year, an eruption of the recurrent nova RS Ophiuchi[2,3] provided the first opportunity to perform comprehensive X-ray observations of such an event and diagnose conditions within the ejecta. Here we show that the hard X-ray emission from RS Ophiuchi early in the eruption emanates from behind a blast wave, or outward-moving shock wave, that expanded freely for less than 2 days and then decelerated due to interaction with the nebula. The X-rays faded rapidly, suggesting that the blast wave deviates from the standard spherical shell structure[4-6]. The early onset of deceleration indicates that the ejected shell had a low mass, the white dwarf has a high mass[7], and that RS Ophiuchi is a progenitor of the type of supernova integral to studies of the expansion of the universe.

  9. THE 2001-2003 LOW STATE OF NOVA LACERTAE 1950 (DK LAC)

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Jacobson, H.; Hoffman, D.; Maxwell, T.; Croxall, K.; Kafka, S.; Henden, A. A.; Robertson, J. W. E-mail: jacob189@msu.edu E-mail: tmaxwell@astro.indiana.edu E-mail: skafka@dtm.ciw.edu E-mail: Jeff.Robertson@atu.edu

    2011-04-15

    We report on extensive photometry of DK Lac obtained during the interval 1990-2009, which includes a 2 mag low state during 2001-2003. Much of the photometry consists of exposures obtained with a typical spacing of several days, but also includes 26 sequences of continuous photometry each lasting 2-7 hr. We find no evidence for periodicities in our data. We do find that the random variations in the low state are approximately twice those in the high state, when expressed in magnitudes. The lack of orbital-timescale variations is attributed to the nearly face-on presentation of the disk. There is a 0.2 mag decline in the high-state brightness of the system over 19 years, which is consistent with the behavior of other old novae in the decades following outburst. High-state spectra are also presented and discussed. We find that the equivalent width of H{alpha} falls by about double from 1991 to 2008. The photometric properties are discussed in the context of the hibernation scenario for the behavior of novae between outbursts, in which we conclude that low states in old novae are probably unrelated to their possible entrance into hibernation.

  10. The 1991-2012 light curve of the old nova HR Lyrae

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Shears, J.; Kafka, S.; Robertson, J. W.; Henden, A. A. E-mail: bunburyobservatory@hotmail.com E-mail: Jeff.Robertson@atu.edu

    2014-05-01

    The 22 yr light curve of HR Lyr, acquired with a typical cadence of 2-6 days, is examined for periodic and quasi-periodic variations. No persistent periodicities are revealed. Rather, the light curve variations often take the form of nearly linear rises and falls having typical e-folding times of about 100 days. Occasional ?0.6 mag outbursts are also seen, with properties similar to those of small outbursts found in some nova-like cataclysmic variables. When the photometry is formed into yearly averages, a decline of 0.012 ± 0.005 mag yr{sup –1} is apparent, consistent with the fading of irradiation-induced M-dot following the nova. The equivalent width of H? is tabulated at three epochs over the interval 1986-2008 in order to compare with a recent result for DK Lac in which H? was found to be fading 50 yr after the nova. However, our results for such a fading in HR Lyr are inconclusive.

  11. Gamma-ray novae as probes of relativistic particle acceleration at non-relativistic shocks

    E-Print Network [OSTI]

    Metzger, Brian D; Vurm, Indrek; Hascoet, Romain; Beloborodov, Andrei M; Chomiuk, Laura

    2015-01-01

    The Fermi LAT discovery that classical novae produce >100 MeV gamma-rays establishes that shocks and relativistic particle acceleration are key features of these events. These shocks are likely to be radiative due to the high densities of the nova ejecta at early times coincident with the gamma-ray emission. Thermal X-rays radiated behind the shock are absorbed by neutral gas and reprocessed into optical emission, similar to Type IIn (interacting) supernovae. The ratio of gamma-ray and optical luminosities, L_gam/L_opt, thus sets a lower limit on the fraction of the shock power used to accelerate relativistic particles, e_nth. The measured values of L_gam/L_opt for two classical novae, V1324 Sco and V339 Del, constrains e_nth > 1e-2 and > 1e-3, respectively. Inverse Compton models for the gamma-ray emission are disfavored given the low electron acceleration efficiency, e_nth ~ 1e-4-1e-3, inferred from observations of Galactic cosmic rays and particle-in-cell (PIC) numerical simulations. Recent hybrid PIC simu...

  12. HUBBLE SPACE TELESCOPE FAR ULTRAVIOLET SPECTROSCOPY OF THE RECURRENT NOVA T PYXIDIS

    SciTech Connect (OSTI)

    Godon, Patrick; Sion, Edward M. [Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States); Starrfield, Sumner [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States); Livio, Mario; Williams, Robert E. [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Woodward, Charles E. [Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN 55455 (United States); Kuin, Paul [Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT (United Kingdom); Page, Kim L., E-mail: patrick.godon@villanova.edu, E-mail: edward.sion@villanova.edu, E-mail: sumner.starrfield@asu.edu, E-mail: mlivio@stsci.edu, E-mail: wms@stsci.edu, E-mail: chelsea@astro.umn.edu, E-mail: n.kuin@ucl.ac.uk, E-mail: klp5@leicester.ac.uk [Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH (United Kingdom)

    2014-04-01

    With six recorded nova outbursts, the prototypical recurrent nova T Pyxidis (T Pyx) is the ideal cataclysmic variable system to assess the net change of the white dwarf mass within a nova cycle. Recent estimates of the mass ejected in the 2011 outburst ranged from a few ?10{sup –5} M {sub ?} to 3.3 × 10{sup –4} M {sub ?}, and assuming a mass accretion rate of 10{sup –8}-10{sup –7} M {sub ?} yr{sup –1} for 44 yr, it has been concluded that the white dwarf in T Pyx is actually losing mass. Using NLTE disk modeling spectra to fit our recently obtained Hubble Space Telescope COS and STIS spectra, we find a mass accretion rate of up to two orders of magnitude larger than previously estimated. Our larger mass accretion rate is due mainly to the newly derived distance of T Pyx (4.8 kpc, larger than the previous 3.5 kpc estimate), our derived reddening of E(B – V) = 0.35 (based on combined IUE and GALEX spectra), and NLTE disk modeling (compared to blackbody and raw flux estimates in earlier works). We find that for most values of the reddening (0.25 ? E(B – V) ? 0.50) and white dwarf mass (0.70 M {sub ?} ? M {sub wd} ? 1.35 M {sub ?}) the accreted mass is larger than the ejected mass. Only for a low reddening (?0.25 and smaller) combined with a large white dwarf mass (0.9 M {sub ?} and larger) is the ejected mass larger than the accreted one. However, the best results are obtained for a larger value of reddening.

  13. MULTIWAVELENGTH PHOTOMETRY AND HUBBLE SPACE TELESCOPE SPECTROSCOPY OF THE OLD NOVA V842 CENTAURUS

    SciTech Connect (OSTI)

    Sion, Edward M. [Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova, PA 19085 (United States); Szkody, Paula; Mukadam, Anjum [Department of Astronomy, University of Washington, Seattle, WA 98195 (United States); Warner, Brian; Woudt, Patrick [Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701 (South Africa); Walter, Frederic [Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794 (United States); Henden, Arne [AAVSO 49 Bay State Road, Cambridge, MA 02138 (United States); Godon, Patrick, E-mail: edward.sion@villanova.edu, E-mail: szkody@astro.washington.edu, E-mail: anjum@astro.washington.edu, E-mail: brian.warner@uct.ac.za, E-mail: pwoudt@ast.uct.ac.za, E-mail: frederick.walter@stonybrook.edu, E-mail: arne@aavso.edu [Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States)

    2013-08-01

    We present ground-based optical and near infrared photometric observations and Hubble Space Telescope (HST) COS spectroscopic observations of the old nova V842 Cen (Nova Cen 1986). Analysis of the optical light curves reveals a peak at 56.5 {+-} 0.3 s with an amplitude of 8.9 {+-} 4.2 mma, which is consistent with the rotation of a magnetic white dwarf primary in V842 Cen that was detected earlier by Woudt et al., and led to its classification as an intermediate polar. However, our UV lightcurve created from the COS time-tag spectra does not show this periodicity. Our synthetic spectral analysis of an HST COS spectrum rules out a hot white dwarf photosphere as the source of the FUV flux. The best-fitting model to the COS spectrum is a full optically thick accretion disk with no magnetic truncation, a low disk inclination angle, low accretion rate and a distance less than half the published distance that was determined on the basis of interstellar sodium D line strengths. Truncated accretion disks with truncation radii of 3 R{sub wd} and 5 R{sub wd} yielded unsatisfactory agreement with the COS data. The accretion rate is unexpectedly low for a classical nova only 24 yr after the explosion when the accretion rate is expected to be high and the white dwarf should still be very hot, especially if irradiation of the donor star took place. Our low accretion rate is consistent with those derived from X-ray and ground-based optical data.

  14. Radio frequency models of novae in eruption. I. The free-free process in bipolar morphologies

    SciTech Connect (OSTI)

    Ribeiro, V. A. R. M.; Simon, T.; Woudt, P. A.; Chomiuk, L.; Munari, U.; Steffen, W.; Koning, N.; O'Brien, T. J.; Bode, M. F.

    2014-09-01

    Observations of novae at radio frequencies provide us with a measure of the total ejected mass, density profile, and kinetic energy of a nova eruption. The radio emission is typically well characterized by the free-free emission process. Most models to date have assumed spherical symmetry for the eruption, although for as long as there have been radio observations of these systems, it has been known that spherical eruptions are too simplistic a geometry. In this paper, we build bipolar models of the nova eruption, assuming the free-free process, and show the effects of varying different parameters on the radio light curves. The parameters considered include the ratio of the minor- to major-axis, the inclination angle, and shell thickness. We also show the uncertainty introduced when fitting spherical-model synthetic light curves to bipolar-model synthetic light curves. We find that the optically thick phase rises with the same power law (S {sub ?}?t {sup 2}) for both the spherical and bipolar models. In the bipolar case, there is a 'plateau' phase—depending on the thickness of the shell as well as the ratio of the minor- to major-axis—before the final decline, which follows the same power law (S {sub ?}?t {sup –3}) as in the spherical case. Finally, fitting spherical models to the bipolar-model synthetic light curves requires, in the worst-case scenario, doubling the ejected mass, more than halving the electron temperature, and reducing the shell thickness by nearly a factor of 10. This implies that in some systems we have been over-predicting the ejected masses and under-predicting the electron temperature of the ejecta.

  15. Detection of a 5-Hz QPO from X-ray Nova GRS 1739-278

    E-Print Network [OSTI]

    K. N. Borozdin; S. P. Trudolyubov

    2000-03-08

    The X-ray nova GRS1739-278 flared up near the Galactic center in the spring of 1996. Here we report on the discovery of a ~5-Hz quasi-periodic oscillations (QPO) in RXTE/PCA observations of GRS1739-278. The QPO were only present when the source was in its very high state, and disappeared later, when it made a transition down into the high state. We present the energy spectra of this black hole candidate measured in both high and very high states, and discuss the similarities between this system and other X-ray transients.

  16. Classical novae and type I X-ray bursts: Challenges for the 21st century

    SciTech Connect (OSTI)

    Parikh, A., E-mail: anuj.r.parikh@upc.edu; José, J., E-mail: jordi.jose@upc.edu; Sala, G., E-mail: gloria.sala@upc.edu [Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya (EUETIB), E-08036 Barcelona (Spain); Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona (Spain)

    2014-04-15

    Classical nova explosions and type I X-ray bursts are the most frequent types of thermonuclear stellar explosions in the Galaxy. Both phenomena arise from thermonuclear ignition in the envelopes of accreting compact objects in close binary star systems. Detailed observations of these events have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. We discuss observational features of these phenomena and theoretical efforts to better understand the energy production and nucleosynthesis in these explosions. We also examine and summarize studies directed at identifying nuclear physics quantities with uncertainties that significantly affect model predictions.

  17. Modeling CHANDRA Low Energy Transmission Grating Spectrometer Observations of Classical Novae with PHOENIX. I. V4743 Sagittarii

    E-Print Network [OSTI]

    Alexander Petz; Peter H. Hauschildt; Jan-Uwe Ness; Sumner Starrfield

    2004-10-15

    We use the PHOENIX code package to model the X-ray spectrum of Nova V4743 Sagittarii observed with the LETGS onboard the Chandra satellite on March 2003. Our atmosphere models are 1D spherical, expanding, line blanketed, and in full NLTE. To analyze nova atmospheres and related systems with an underlying nuclear burning envelope at X-ray wavelengths, it was necessary to update the code with new microphysics, as discussed in this paper. We demonstrate that the X-ray emission is dominated by thermal bremsstrahlung and that the hard X-rays are dominated by Fe and N absorption. The best fit to the observation is provided at a temperature of T_eff = 5.8 x 10^5 K, with L_bol = 50 000 L_sun. The models are calculated for solar abundances. It is shown that the models can be used to determine abundances in the nova ejecta.

  18. HST Fine Guidance Sensor Astrometric Parallaxes for Three Dwarf Novae: SS Aurigae, SS Cygni, and U Geminorum

    E-Print Network [OSTI]

    Thomas E. Harrison; Bernard J. McNamara; Paula Szkody; Barbara J. McAurthur; G. F. Benedict; Arnold R. Klemola; Ronald L. Gilliland

    1999-02-16

    We report astrometric parallaxes for three well known dwarf novae obtained using the Fine Guidance Sensors on the Hubble Space Telescope. We found a parallax for SS Aurigae of Pi = 5.00 +/- 0.64 mas, for SS Cygni we found Pi = 6.02 +/- 0.46 mas, and for U Geminorum we obtained Pi = 10.37 +/- 0.50 mas. These represent the first true trigonometric parallaxes of any dwarf novae. We briefly compare these results with previous distance estimates. This program demonstrates that with a very modest amount of HST observing time, the Fine Guidance Sensors can deliver parallaxes of unrivaled precision.

  19. GRB 080503 late afterglow re-brightening: signature of a magnetar powered merger-nova

    E-Print Network [OSTI]

    Gao, He; Wu, Xue-Feng; Dai, Zi-Gao; Zhang, Bing

    2015-01-01

    GRB 080503 is a short gamma-ray burst (GRB) detected by \\emph{Swift} and has been classified as a compact-star-merger-origin GRB. The soft extended emission and the simultaneous late re-brightening in both the X-ray and optical afterglow lightcurves raise interesting questions regarding its physical origin. We show that the broad-band data of GRB 080503 can be well explained within the framework of the double neutron star merger model, provided that the merger remnant is a rapidly-rotating massive neutron star with an extremely high magnetic field (i.e. a millisecond magnetar). We show that the late optical re-brightening is consistent with the emission from a magnetar-powered "merger-nova". This adds one more case to the growing sample of merger-novae associated with short GRBs. The soft extended emission and the late X-ray excess emission are well connected through a magnetar dipole spin-down luminosity evolution function, suggesting that direct magnetic dissipation is the mechanism to produce these X-rays....

  20. Short-period X-ray oscillations in super-soft novae and persistent SSS

    E-Print Network [OSTI]

    Ness, J -U; Osborne, J P; Kuulkers, E; Henze, M; Piro, A L; Drake, J J; Dobrotka, A; Schwarz, G; Starrfield, S; Kretschmar, P; Hirsch, M; Wilms, J

    2015-01-01

    Transient short-period <100s oscillations have been found in the X-ray light curves of three novae during their SSS phase and in one persistent SSS. We pursue an observational approach to determine possible driving mechanisms and relations to fundamental system parameters such as the white dwarf mass. We performed a systematic search for short-period oscillations in all available XMM-Newton and Chandra X-ray light curves of persistent SSS and novae during their SSS phase. To study time evolution, we divided each light curve into short time segments and computed power spectra. We then constructed dynamic power spectra from which we identified transient periodic signals even when only present for a short time. From all time segments of each system, we computed fractions of time when periodic signals were detected. In addition to the previously known systems with short-period oscillations, RS Oph (35s), KT Eri (35s), V339 Del (54s), and Cal 83 (67s), we found one additional system, LMC 2009a (33s), and also c...

  1. Suzaku observation of the classical nova V2491 Cyg in quiescence

    E-Print Network [OSTI]

    Zemko, Polina; Orio, Marina

    2015-01-01

    We present Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that either we observe remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate "soft intermediate polar". We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The later is typical of intermediate polars. The X-ray light-curve shows a modulation with a $\\sim$38 min period. The amplitude of this modulation is strongly energy dependent and reaches maximum in the 0.8--2.0 keV range. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario.

  2. X-Ray Spectroscopy of the Classical Nova V458 Vulpeculae with Suzaku

    E-Print Network [OSTI]

    Tsujimoto, Masahiro; Drake, Jeremy J; Ness, Jan-Uwe; Kitamoto, Shunji

    2008-01-01

    We conducted a target of opportunity X-ray observation of the classical nova V458 Vulpeculae 88 days after the explosion using the Suzaku satellite. With a 20 ks exposure, the X-ray Imaging Spectrometer detected X-ray emission significantly harder than typical super-soft source emission. The X-ray spectrum shows K lines from N, Ne, Mg, Si, and S, and L-series emission from Fe in highly ionized states. The spectrum can be described by a single temperature (0.64 keV) thin thermal plasma model in collisional equilibrium with a hydrogen-equivalent extinction column density of ~3e21/cm2, a flux of ~1e-12 erg/s/cm2, and a luminosity of ~6e34 erg/s in the 0.3-3.0 keV band at an assumed distance of 13 kpc. We found a hint of an enhancement of N and deficiencies of O and Fe relative to other metals. The observed X-ray properties can be interpreted as the emission arising from shocks of ejecta from an ONe-type nova.

  3. Photoionization Heating of Nova Ejecta by the Post-Outburst Supersoft Source

    E-Print Network [OSTI]

    Cunningham, Timothy; Bildsten, Lars

    2015-01-01

    The expanding ejecta from a classical nova remains hot enough ($\\sim10^{4}\\, {\\rm K}$) to be detected in thermal radio emission for up to years after the cessation of mass loss triggered by a thermonuclear instability on the underlying white dwarf (WD). Nebular spectroscopy of nova remnants confirms the hot temperatures observed in radio observations. During this same period, the unstable thermonuclear burning transitions to a prolonged period of stable burning of the remnant hydrogen-rich envelope, causing the WD to become, temporarily, a super-soft X-ray source. We show that photoionization heating of the expanding ejecta by the hot WD maintains the observed nearly constant temperature of $(1-4)\\times10^4\\mathrm{~K}$ for up to a year before an eventual decline in temperature due to either the cessation of the supersoft phase or the onset of a predominantly adiabatic expansion. We simulate the expanding ejecta using a one-zone model as well as the Cloudy spectral synthesis code, both incorporating the time-d...

  4. MULTIPLICITY OF NOVA ENVELOPE SOLUTIONS AND OCCURRENCE OF OPTICALLY THICK WINDS

    SciTech Connect (OSTI)

    Kato, Mariko; Hachisu, Izumi E-mail: hachisu@ea.c.u-tokyo.ac.jp

    2009-07-10

    We revisit the occurrence condition of optically thick winds reported by Kato in 1985 and Kato and Hachisu in 1989 who mathematically examined nova envelope solutions with an old opacity and found that optically thick winds are accelerated only in massive white dwarfs (WDs) of {approx}>0.9 M{sub sun}. With the OPAL opacity we find that the optically thick wind occurs for {approx}>0.6 M{sub sun} WDs and that the occurrence of winds depends not only on the WD mass but also on the ignition mass. When the ignition mass is larger than a critical value, winds are suppressed by a density-inversion layer. Such a static solution can be realized in WDs of mass {approx}0.6-0.7 M{sub sun}. We propose that sequences consisting only of static solutions correspond to slow evolutions in symbiotic novae like PU Vul because PU Vul shows no indication of strong winds in a long-lasted flat peak followed by a very slow decline in its light curve.

  5. X-Ray Spectroscopy of the Classical Nova V458 Vulpeculae with Suzaku

    E-Print Network [OSTI]

    Masahiro Tsujimoto; Dai Takei; Jeremy J. Drake; Jan-Uwe Ness; Shunji Kitamoto

    2008-10-17

    We conducted a target of opportunity X-ray observation of the classical nova V458 Vulpeculae 88 days after the explosion using the Suzaku satellite. With a 20 ks exposure, the X-ray Imaging Spectrometer detected X-ray emission significantly harder than typical super-soft source emission. The X-ray spectrum shows K lines from N, Ne, Mg, Si, and S, and L-series emission from Fe in highly ionized states. The spectrum can be described by a single temperature (0.64 keV) thin thermal plasma model in collisional equilibrium with a hydrogen-equivalent extinction column density of ~3e21/cm2, a flux of ~1e-12 erg/s/cm2, and a luminosity of ~6e34 erg/s in the 0.3-3.0 keV band at an assumed distance of 13 kpc. We found a hint of an enhancement of N and deficiencies of O and Fe relative to other metals. The observed X-ray properties can be interpreted as the emission arising from shocks of ejecta from an ONe-type nova.

  6. Quantifying atmospheric pollution across north america from boreal forest fires: a combined analysis of atmospheric modelling and ground-based remote sensing 

    E-Print Network [OSTI]

    Trigwell, Robert

    2011-11-24

    This paper describes the interpretation of the 2010 summer LIDAR observations from Dal- housie University, Nova Scotia. The GEOS-Chem global 3D chemistry transport model was used to identify the chemical and optical ...

  7. Title: Satellite Streetview: Canadian Cities and Regions Data Creator /

    E-Print Network [OSTI]

    , Hamilton, Kitchener, St. Catharines, Quebec City, Montreal, Jonquiere, Halifax, Fredericton, St. Johns, Ontario; Cornwall, Ontario; Hamilton, Ontario; Kitchener, Ontario; St, Catherines, Ontario; Quebec City, Quebec; Montreal, Quebec; Jonquiere, Quebec; Halifax, Nova Scotia; Fredericton, New Brunswick; St. John

  8. DOE/CETC/CANDRA Workshop on Microturbine Applications January 21-23, 2003 ~ Calgary, Alberta, Canada

    E-Print Network [OSTI]

    Pennycook, Steve

    Energy General Hospital 30 kW Mariah CHP operating on Light Fuel Oil Chuck Faulkner, Nova Scotia Power Inc Alliance Canada #12;January 21 DOE/CETC/CANDRA Workshop on Microturbine Applications Agenda Wednesday

  9. Teaching Humanities in Medicine: The University of Massachusetts Family Medicine Residency Program Experience

    E-Print Network [OSTI]

    Silk, Hugh; Shields, Sara

    2012-01-01

    Charon R. Narrative and medicine. N Eng J Med 2004;350:862-California, Irvine, College of Medicine. Acad Med. 2003;78:University Faculty of Medicine, Nova Scotia, Canada, 1992–

  10. 46 Marine Fisheries Review Introduction

    E-Print Network [OSTI]

    , three companies, one in Massachusetts, one in New Brunswick, and one on Prince Edward Island, Canada), Scotland (Edwards, 1997), and in Atlantic Canada (Quebec, New- foundland, Nova Scotia), and also St. Pierre

  11. American Fisheries Society Symposium 79:185203, 2012 2012 by the American Fisheries Society

    E-Print Network [OSTI]

    Townsend, David W.

    of Oceanography Post Office Box 1006, 1 Challenger Drive, Dartmouth, Nova Scotia B2Y 4A2, Canada Neal r. Pettigrew of Oceanography Post Office Box 1006, Dartmouth, Nova Scotia B2Y 4A2, Canada DaviD w. towNSeND School of Marine Sciences, University of Maine Orono, Maine 04469, USA guoqi haN Northwest Atlantic Fisheries Center Post

  12. The 2011 outburst of recurrent nova T PYX: Radio observations reveal the ejecta mass and hint at complex mass loss

    SciTech Connect (OSTI)

    Nelson, Thomas [School of Physics and Astronomy, University of Minnesota, 116 Church St. SE, Minneapolis, MN 55455 (United States); Chomiuk, Laura [Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States); Roy, Nirupam; Krauss, Miriam I.; Mioduszewski, Amy J.; Rupen, Michael P. [National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801 (United States); Sokoloski, J. L.; Weston, Jennifer [Columbia Astrophysics Laboratory, Columbia University, New York, NY (United States); Mukai, Koji, E-mail: tnelson@physics.umn.edu [Center for Space Science and Technology, University of Maryland Baltimore County, Baltimore, MD 21250 (United States)

    2014-04-10

    Despite being the prototype of its class, T Pyx is arguably the most unusual and poorly understood recurrent nova. Here, we use radio observations from the Karl G. Jansky Very Large Array to trace the evolution of the ejecta over the course of the 2011 outburst of T Pyx. The radio emission is broadly consistent with thermal emission from the nova ejecta. However, the radio flux began rising surprisingly late in the outburst, indicating that the bulk of the radio-emitting material was either very cold, or expanding very slowly, for the first ?50 days of the outburst. Considering a plausible range of volume filling factors and geometries for the ejecta, we find that the high peak flux densities of the radio emission require a massive ejection of (1-30) × 10{sup –5} M {sub ?}. This ejecta mass is much higher than the values normally associated with recurrent novae, and is more consistent with a nova on a white dwarf well below the Chandrasekhar limit.

  13. Getting the most from NOvA and T2K

    SciTech Connect (OSTI)

    Mena, Olga; /Fermilab

    2006-09-01

    The determination of the ordering of the neutrino masses (the hierarchy) is probably a crucial prerequisite to understand the origin of lepton masses and mixings and to establish their relationship to the analogous properties in the quark sector. In this talk, we follow an alternative strategy to the usual neutrino-antineutrino comparison: we exploit the combination of the neutrino-only data from the NOvA and the T2K experiments by performing these two off-axis experiments at different distances but at the same /L, being the mean neutrino energy and L the baseline. This would require a minor adjustment to the proposed off-axis angle for one or both of the proposed experiments.

  14. NOvA and T2K: The Race for the neutrino mass hierarchy

    SciTech Connect (OSTI)

    Mena, Olga; /Fermilab; Nunokawa, Hiroshi; /Rio de Janeiro, Pont. U. Catol.; Parke, Stephen J.; /Fermilab

    2006-09-01

    The determination of the ordering of the neutrino masses (the hierarchy) is probably a crucial prerequisite to understand the origin of lepton masses and mixings and to establish their relationship to the analogous properties in the quark sector. Here, we follow an alternative strategy to the usual neutrino-antineutrino comparison in long baseline neutrino oscillation experiments: we exploit the combination of the neutrino-only data from the NOvA and the T2K experiments by performing these two off-axis experiments at different distances but at the same /L, where is the mean neutrino energy and L is the baseline. This would require a minor adjustment to the proposed off-axis angle for one or both of the proposed experiments.

  15. BRIGHT 'MERGER-NOVA' FROM THE REMNANT OF A NEUTRON STAR BINARY MERGER: A SIGNATURE OF A NEWLY BORN, MASSIVE, MILLISECOND MAGNETAR

    SciTech Connect (OSTI)

    Yu, Yun-Wei [Institute of Astrophysics, Central China Normal University, Wuhan 430079 (China)] [Institute of Astrophysics, Central China Normal University, Wuhan 430079 (China); Zhang, Bing; Gao, He, E-mail: yuyw@mail.ccnu.edu.cn, E-mail: zhang@physics.unlv.edu [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States)] [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States)

    2013-10-20

    A massive millisecond magnetar may survive the merger of a neutron star (NS) binary, which would continuously power the merger ejecta. We develop a generic dynamic model for the merger ejecta with energy injection from the central magnetar. The ejecta emission (the {sup m}erger-nova{sup )} powered by the magnetar peaks in the UV band and the peak of the light curve, progressively shifts to an earlier epoch with increasing frequency. A magnetar-powered merger-nova could have an optical peak brightness comparable to a supernova, which is a few tens or hundreds times brighter than the radioactive-powered merger-novae (the so-called macro-nova or kilo-nova). On the other hand, such a merger-nova would peak earlier and have a significantly shorter duration than that of a supernova. An early collapse of the magnetar could suppress the brightness of the optical emission and shorten its duration. Such millisecond-magnetar-powered merger-novae may be detected from NS-NS merger events without an observed short gamma-ray burst, and could be a bright electromagnetic counterpart for gravitational wave bursts due to NS-NS mergers. If detected, it suggests that the merger leaves behind a massive NS, which has important implications for the equation-of-state of nuclear matter.

  16. Non-LTE model atmosphere analysis of the early ultraviolet spectra of nova OS Andromedae 1986

    E-Print Network [OSTI]

    Greg Schwarz; Peter H. Hauschildt; Sumner Starrfield; Eddie Baron; France Allard; Steve Shore; George Sonneborn

    1996-08-29

    We have analyzed the early optically thick ultraviolet spectra of Nova OS And 1986 using a grid of spherically symmetric, non-LTE, line-blanketed, expanding model atmospheres and synthetic spectra with the following set of parameters: $5,000\\le$ T$_{model}$ $\\le 60,000$K, solar abundances, $\\rho \\propto r^{-3}$, $\\v_{max} = 2000\\kms$, $L=6 \\times 10^{4}\\Lsun$, and a statistical or microturbulent velocity of 50 $\\kms$. We used the synthetic spectra to estimate the model parameters corresponding to the observed {\\it IUE} spectra. The fits to the observations were then iteratively improved by changing the parameters of the model atmospheres, in particular T$_{model}$ and the abundances, to arrive at the best fits to the optically thick pseudo-continuum and the features found in the {\\it IUE} spectra. The {\\it IUE} spectra show two different optically thick subphases. The earliest spectra, taken a few days after maximum optical light, show a pseudo-continuum created by overlapping absorption lines. The later observations, taken approximately 3 weeks after maximum light, show the simultaneous presence of allowed, semi-forbidden, and forbidden lines in the observed spectra. Analysis of these phases indicate that OS And 86 had solar metallicities except for Mg which showed evidence of being underabundant by as much as a factor of 10. We determine a distance of 5.1 kpc to OS And 86 and derive a peak bolometric luminosity of $\\sim$ 5 $\\times$ 10$^4$ L$_{\\odot}$. The computed nova parameters provide insights into the physics of the early outburst and explain the spectra seen by {\\it IUE}. Lastly, we find evidence in the later observations for large non-LTE effects of Fe{\\sc ii} which, when included, lead to much better agreement with the observations.

  17. Discovery of $^{34g,m}$Cl$(p,?)^{35}$Ar resonances activated at classical nova temperatures

    E-Print Network [OSTI]

    C. Fry; C. Wrede; S. Bishop; B. A. Brown; A. A. Chen; T. Faestermann; R. Hertenberger; A. Parikh; D. Pérez-Loureiro; H. -F. Wirth; A. García; R. Ortez

    2015-10-14

    Background: The thermonuclear $^{34g,m}$Cl($p,\\gamma$)$^{35}$Ar reaction rates are unknown due to a lack of experimental nuclear physics data. Uncertainties in these rates translate to uncertainties in $^{34}$S production in models of classical novae on oxygen-neon white dwarfs. $^{34}$S abundances have the potential to aid in the classification of presolar grains. Purpose: Determine resonance energies for the $^{34g,m}$Cl($p,\\gamma$)$^{35}$Ar reactions within the region of astrophyical interest for classical novae to a precision of a few keV as an essential first step toward constraining their thermonuclear reaction rates. Method: $^{35}$Ar excited states were populated by the $^{36}$Ar($d,t$)$^{35}$Ar reaction at $E$(d)=22~MeV and reaction products were momentum analyzed by a high resolution quadrupole-dipole-dipole-dipole (Q3D) magnetic spectrograph. Results: Seventeen new $^{35}$Ar levels have been detected at a statistically significant level in the region $E_x\\approx$~5.9-6.7~MeV ($E_r$ \\textless~800~ keV) and their excitation energies have been determined to typical uncertainties of 3~keV. The uncertainties for five previously known levels have also been reduced substantially. The measured level density was compared to those calculated using the WBMB Hamiltonian within the $sd-pf$ model space. Conclusions: Most of the resonances in the region of astrophyical interest have likely been discovered and their energies have been determined, but the resonance strengths are still unknown, and experimentally constraining the $^{34g,m}$Cl($p,\\gamma$)$^{35}$Ar reaction rates will require further experiments.

  18. FROM X-RAY DIPS TO ECLIPSE: WITNESSING DISK REFORMATION IN THE RECURRENT NOVA U Sco

    SciTech Connect (OSTI)

    Ness, J.-U.; Talavera, A.; Gonzalez-Riestra, R. [XMM-Newton Science Operations Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada, Madrid (Spain); Schaefer, B. E. [Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803 (United States); Dobrotka, A. [Department of Physics, Institute of Materials Science, Faculty of Materials Science and Technology, Slovak University of Technology, Jana Bottu 25, 91724 Trnava (Slovakia); Sadowski, A. [N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa (Poland); Drake, J. J.; Barnard, R. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Page, K. L. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Hernanz, M. [Institut de Ciencies de l'Espai (CSIC-IEEC), Campus UAB, Facultat de Ciencies, C5 parell 2on, 08193 Bellaterra (Barcelona) (Spain); Sala, G. [Departament Fisica i Enginyeria Nuclear, EUETIB (UPC-IEEC), Comte d'Urgell 187, 08036 Barcelona (Spain); Starrfield, S., E-mail: juness@sciops.esa.int [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 (United States)

    2012-01-20

    The tenth recorded outburst of the recurrent eclipsing nova U Sco was observed simultaneously in X-ray, UV, and optical by XMM-Newton on days 22.9 and 34.9 after the outburst. Two full passages of the companion in front of the nova ejecta were observed, as was the reformation of the accretion disk. On day 22.9, we observed smooth eclipses in UV and optical but deep dips in the X-ray light curve that disappeared by day 34.9, yielding clean eclipses in all bands. X-ray dips can be caused by clumpy absorbing material that intersects the line of sight while moving along highly elliptical trajectories. Cold material from the companion could explain the absence of dips in UV and optical light. The disappearance of X-ray dips before day 34.9 implies significant progress in the formation of the disk. The X-ray spectra contain photospheric continuum emission plus strong emission lines, but no clear absorption lines. Both continuum and emission lines in the X-ray spectra indicate a temperature increase from day 22.9 to day 34.9. We find clear evidence in the spectra and light curves for Thompson scattering of the photospheric emission from the white dwarf. Photospheric absorption lines can be smeared out during scattering in a plasma of fast electrons. We also find spectral signatures of resonant line scattering that lead to the observation of the strong emission lines. Their dominance could be a general phenomenon in high-inclination systems such as Cal 87.

  19. Scotia Wind Ltd | 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 J APPENDIX E LIST OFAMERICA'SHeavyAgency (IRENA)OptionsEquivalentBScira Offshore Energy Jump

  20. Full aperture backscatter station imager diagnostics system for far-field imaging of laser plasma instabilities on Nova

    SciTech Connect (OSTI)

    Wilke, M.D.; Fernandez, J.C.; Berggren, R.R.; Horton, R.F.; Montgomery, D.S.; Faulkner, J.A.; Looney, L.D.; Jimerson, J.R.

    1997-01-01

    In ICF, the understanding of laser plasma scattering processes is essential for laser target coupling and for controlling the symmetry of indirect drive implosions. The existing Nova full aperture backscatter station has been useful in understanding laser plasma instabilities occurring in hohlraums by measuring the quantity, spectral distribution, and near-field spatial distributions of Brillouin and more recently Raman backscatter. Equally important is an understanding of the far-field spatial intensity distribution which could help in understanding filamentation, threshold and saturation processes. This article describes a broadband, color-corrected far-field imager and associated diagnostics capable of imaging the source of scattered light to better than 25 {mu}m resolution. Brillouin and Raman backscatter can be imaged through the Nova beam-7 focusing lens or the imager can be used like a microscope to image side scatter from other beams. {copyright} {ital 1997 American Institute of Physics.}

  1. Direct measurements of 22Na(p,g)23Mg resonances and consequences for 22Na production in classical novae

    E-Print Network [OSTI]

    A. L. Sallaska; C. Wrede; A. Garcia; D. W. Storm; T. A. D. Brown; C. Ruiz; K. A. Snover; D. F. Ottewell; L. Buchmann; C. Vockenhuber; D. A. Hutcheon; J. A. Caggiano

    2010-09-24

    The radionuclide 22Na is a potential astronomical observable that is expected to be produced in classical novae in quantities that depend on the thermonuclear rate of the 22Na(p,g)23Mg reaction. We have measured the strengths of low-energy 22Na(p,g)23Mg resonances directly and absolutely using a radioactive 22Na target. We find the strengths of resonances at E_p = 213, 288, 454, and 610 keV to be higher than previous measurements by factors of 2.4 to 3.2, and we exclude important contributions to the rate from proposed resonances at E_p = 198, 209, and 232 keV. The 22Na abundances expected in the ejecta of classical novae are reduced by a factor of ~ 2.

  2. On the 21Na(p,gamma)22Mg thermonuclear rate for 22Na production in novae

    E-Print Network [OSTI]

    Nadya A. Smirnova; Alain Coc

    2000-08-16

    Classical novae are potential sources of gamma-rays, like the 1.275 MeV gamma emission following 22Na beta decay, that could be detected by appropriate instruments on board of future satellites like INTEGRAL. It has been shown that the production of 22Na by novae is affected by the uncertainty on the 21Na(p,gamma)22Mg rate and in particular by the unknown partial widths of the Ex = 5.714 MeV, J^pi = 2^+, 22Mg level. To reduce these uncertainties, we performed shell model calculations with the OXBASH code, compared the results with available spectroscopic data and calculated the missing partial widths. Finally, we discuss the influence of these results on the 21Na(p,gamma)22Mg reaction rate and 22Na synthesis.

  3. XMM-Newton observations of the dwarf nova RU Peg in quiescence: Probe of the boundary layer

    E-Print Network [OSTI]

    Balman, S; Sion, E M; Ness, J -U; Schlegel, E; Barrett, P E; Szkody, P

    2011-01-01

    We present an analysis of X-ray and UV data obtained with the XMM-Newton Observatory of the long period dwarf nova RU Peg. RU Peg contains a massive white dwarf, possibly the hottest white dwarf in a dwarf nova, it has a low inclination, thus optimally exposing its X-ray emitting boundary layer, and has an excellent trigonometric parallax distance. We modeled the X-ray data using XSPEC assuming a multi-temperature plasma emission model built from the MEKAL code. We obtained a maximum temperature of 31.7 keV, based on the EPIC MOS1, 2 and pn data, indicating that RU Peg has an X-ray spectrum harder than most dwarf novae, except U Gem. This result is consistent with and indirectly confirms the large mass of the white dwarf in RU Peg. The X-ray luminosity we computed corresponds to a boundary layer luminosity for a mass accretion rate of 2.E-11 Msun/yr (assuming Mwd=1.3Msun), in agreement with an expected quiescent accretion rate. The modeling of the O VIII emission line at 19A as observed by the RGS implies a p...

  4. Dwarf Nova-like Outburst of Short Period Intermediate Polar HT Camelopardalis

    E-Print Network [OSTI]

    Ryoko Ishioka; Taichi Kato; Makoto Uemura; Gary W. Billings; Koichi Morikawa; Ken'ichi Torii; Kenji Tanabe; Arto Oksanen; Harri Hyvonen; Hitoshi Itoh

    2002-06-12

    We report the first time-series observations of the short outburst of the proposed intermediate polar HT Cam (=RX J0757.0+6306). On 2001 December 29, we detected the object was undergoing a bright outburst at the magnitude of $m_{vis}=12.2$. Following this detection, we started international joint observations through VSNET. The light curve showed a gradual decline for the first 0.5 d. Following this short plateau phase, the rate of decline dramatically increased to more than 4 mag d$^{-1}$. Within 1.5 d from the outburst detection, the object almost declined to the quiescent level. During the rapidly declining phase, long-term modulations with a period of 86 min and strong pulses with a period of 8.6 min were observed. We concluded that 86 min and 8.6 min are the orbital period and the spin period of HT Cam, respectively. By the detection of the spin period, we confirmed the IP classification of HT Cam. However, its outburst behavior rather resembles that of dwarf novae. The discrepancy between the declining rates of the total flux and the pulse flux strongly suggests that the disk instabilities were taking place during the outburst.

  5. THE SUPERSOFT X-RAY PHASE OF NOVA RS OPHIUCHI 2006

    SciTech Connect (OSTI)

    Osborne, J. P.; Page, K. L.; Beardmore, A. P.; Goad, M. R.; Bode, M. F.; O'Brien, T. J.; Starrfield, S.; Rauch, T.; Ness, J.-U.; Krautter, J.; Schwarz, G.; Burrows, D. N.; Gehrels, N.; Drake, J. J.; Evans, A.; Eyres, S. P. S.

    2011-02-01

    Swift X-ray observations of the {approx}60 day supersoft phase of the recurrent nova RS Ophiuchi (RS Oph) 2006 show the progress of nuclear burning on the white dwarf (WD) in exquisite detail. First seen 26 days after the optical outburst, this phase started with extreme variability likely due to variable absorption, although intrinsic WD variations are not excluded. About 32 days later, a steady decline in count rate set in. NLTE model atmosphere spectral fits during the supersoft phase show that the effective temperature of the WD increases from {approx}65 eV to {approx}90 eV during the extreme variability phase, falling slowly after about day 60 and more rapidly after day 80. The bolometric luminosity is seen to be approximately constant and close to Eddington from day 45 up to day 60, the subsequent decline possibly signaling the end of extensive nuclear burning. Before the decline, a multiply-periodic {approx}35 s modulation of the soft X-rays was present and may be the signature of a nuclear fusion driven instability. Our measurements are consistent with a WD mass near the Chandrasekhar limit; combined with a deduced accumulation of mass transferred from its binary companion, this leads us to suggest that RS Oph is a strong candidate for a future supernova explosion. The main uncertainty now is whether the WD is the CO type necessary for a Type Ia supernova. This may be confirmed by detailed abundance analyses of spectroscopic data from the outbursts.

  6. Spectroscopic Study of the Envelope of the Hybrid Nova V458 Vul and Surrounding Nebula

    E-Print Network [OSTI]

    Tarasova, T N

    2015-01-01

    Spectroscopic observations of the hybrid V458 Vul obtained between days 9 and 778 after the brightness maximum are analyzed. Short-period, daily profile variations of forbidden [FeVII] iron lines were detected in the nebular phase, as well as a long-period (about 60-day) cyclic variation that was correlated with the photometric and X-ray cycles. The abundances of helium, neon, and iron in the nova's envelope have been estimated. The helium, neon, and iron abundances exceed the solar values by factors of 4.4, 4.8, and 3.7. The envelope mass is 1.4$\\times$ 10$^{-5}$M$_{\\odot}$. The electron temperatures and number densities have been calculated for the Northwestern and Southeastern knots of the planetary nebula. The temperature derived for the Northwestern knot is Te = 10 000 K and the electron number density, n$_{e}$ = 600 cm $^{-3}$ for the Southeastern knot, Te = 13 000 K and n$_{e}$ = 750 cm$^{-3}$.

  7. X-ray Development of the Classical Nova V2672 Ophiuchi with Suzaku

    E-Print Network [OSTI]

    Takei, D; Drake, J J; Kitamoto, S

    2013-01-01

    We report the Suzaku detection of a rapid flare-like X-ray flux amplification early in the development of the classical nova V2672 Ophiuchi. Two target-of-opportunity ~25 ks X-ray observations were made 12 and 22 days after the outburst. The flux amplification was found in the latter half of day 12. Time-sliced spectra are characterized by a growing supersoft excess with edge-like structures and a relatively stable optically-thin thermal component with Ka emission lines from highly ionized Si. The observed spectral evolution is consistent with a model that has a time development of circumstellar absorption, for which we obtain the decline rate of ~10-40 % in a time scale of 0.2 d on day 12. Such a rapid drop of absorption and short-term flux variability on day 12 suggest inhomogeneous ejecta with dense blobs/holes in the line of sight. Then on day 22 the fluxes of both supersoft and thin-thermal plasma components become significantly fainter. Based on the serendipitous results we discuss the nature of this so...

  8. The Relationship Between X-ray Luminosity and Duty Cycle for Dwarf Novae and their Specific Frequency in the Inner Galaxy

    E-Print Network [OSTI]

    Britt, C T; Pretorius, M L; Hynes, R I; Jonker, P G; Torres, M A P; Knigge, C; Heinke, C O; Johnson, C B; Steeghs, D; Greiss, S; Nelemans, G

    2015-01-01

    We measure the duty cycles for an existing sample of well observed, nearby dwarf novae using data from AAVSO, and present a quantitative empirical relation between the duty cycle of dwarf novae outbursts and the X-ray luminosity of the system in quiescence. We have found that $\\log DC=0.63(\\pm0.21)\\times(\\log L_{X}({\\rm erg\\,s^{-1}})-31.3)-0.95(\\pm0.1)$, where DC stands for duty cycle. We note that there is intrinsic scatter in this relation greater than what is expected from purely statistical errors. Using the dwarf nova X-ray luminosity functions from \\citet{Pretorius12} and \\citet{Byckling10}, we compare this relation to the number of dwarf novae in the Galactic Bulge Survey which were identified through optical outbursts during an 8-day long monitoring campaign. We find a specific frequency of X-ray bright ($L_{X}>10^{31}\\,{\\rm erg\\,s^{-1}}$) Cataclysmic Variables undergoing Dwarf Novae outbursts in the direction of the Galactic Bulge of $6.6\\pm4.7\\times10^{-5}\\,M_{\\odot}^{-1}$. Such a specific frequency...

  9. The 2011 outburst of recurrent nova T Pyx: X-ray observations expose the white dwarf mass and ejection dynamics

    SciTech Connect (OSTI)

    Chomiuk, Laura [Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States); Nelson, Thomas [School of Physics and Astronomy, University of Minnesota, 115 Church Street SE, Minneapolis, MN 55455 (United States); Mukai, Koji [CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771 (United States); Sokoloski, J. L.; Weston, Jennifer [Columbia Astrophysics Laboratory, Columbia University, New York, NY (United States); Rupen, Michael P.; Mioduszewski, Amy J.; Krauss, Miriam I. [National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801 (United States); Page, Kim L.; Osborne, Julian P. [Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH (United Kingdom); Kuulkers, Erik [European Space Astronomy Centre (ESA/ESAC), Science Operations Department, E-28691 Villanueva de la Caada, Madrid (Spain); Roy, Nirupam, E-mail: chomiuk@pa.msu.edu [Max Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany)

    2014-06-20

    The recurrent nova T Pyx underwent its sixth historical outburst in 2011, and became the subject of an intensive multi-wavelength observational campaign. We analyze data from the Swift and Suzaku satellites to produce a detailed X-ray light curve augmented by epochs of spectral information. X-ray observations yield mostly non-detections in the first four months of outburst, but both a super-soft and hard X-ray component rise rapidly after Day 115. The super-soft X-ray component, attributable to the photosphere of the nuclear-burning white dwarf, is relatively cool (?45 eV) and implies that the white dwarf in T Pyx is significantly below the Chandrasekhar mass (?1 M {sub ?}). The late turn-on time of the super-soft component yields a large nova ejecta mass (? 10{sup –5} M {sub ?}), consistent with estimates at other wavelengths. The hard X-ray component is well fit by a ?1 keV thermal plasma, and is attributed to shocks internal to the 2011 nova ejecta. The presence of a strong oxygen line in this thermal plasma on Day 194 requires a significantly super-solar abundance of oxygen and implies that the ejecta are polluted by white dwarf material. The X-ray light curve can be explained by a dual-phase ejection, with a significant delay between the first and second ejection phases, and the second ejection finally released two months after outburst. A delayed ejection is consistent with optical and radio observations of T Pyx, but the physical mechanism producing such a delay remains a mystery.

  10. Direct measurement of the 15N(p,gamma)16O total cross section at novae energies

    E-Print Network [OSTI]

    D Bemmerer; A Caciolli; R Bonetti; C Broggini; F Confortola; P Corvisiero; H Costantini; Z Elekes; A Formicola; Zs Fulop; G Gervino; A Guglielmetti; C Gustavino; Gy Gyurky; M Junker; B Limata; M Marta; R Menegazzo; P Prati; V Roca; C Rolfs; C Rossi Alvarez; E Somorjai; O Straniero

    2009-02-04

    The 15N(p,gamma)16O reaction controls the passage of nucleosynthetic material from the first to the second carbon-nitrogen-oxygen (CNO) cycle. A direct measurement of the total 15N(p,gamma)16O cross section at energies corresponding to hydrogen burning in novae is presented here. Data have been taken at 90-230 keV center-of-mass energy using a windowless gas target filled with nitrogen of natural isotopic composition and a bismuth germanate summing detector. The cross section is found to be a factor two lower than previously believed.

  11. Observational Accuracy of Variable Stars, Novae and Supernovae from Naked Eye to General Relativistic Standard: a Balance over Thousand SGQ Observations Sent to AAVSO

    E-Print Network [OSTI]

    Sigismondi, Costantino

    2015-01-01

    The theory of General Relativity deals with very accurate measurements that show significant divergences from Newtonian predictions only with speeds near to the velocity of light. An introduction for educational purposes, based on naked eye photometry, deals with the radiation near collapsing star's shells like novae and supernovae. The theme of accuracy is drafted from entry level observations to the precision of professional data, often of public domain on the web. Thousand observations of variable stars, included the type 1a SN2014J, the Nova Del 2013 and the Nova Cen 2013, sent to the AAVSO by the author, with SGQ code, during the period 1998-2015 are analyzed to increase the photometric accuracy, in the occasion of the International Year of Light 2015.

  12. New 34Cl proton-threshold states and the thermonuclear 33S(p,gamma)34Cl rate in ONe novae

    E-Print Network [OSTI]

    A. Parikh; T. Faestermann; R. Hertenberger; R. Kruecken; D. Schafstadler; H. -F. Wirth; T. Behrens; V. Bildstein; S. Bishop; K. Eppinger; C. Herlitzius; C. Hinke; M. Schlarb; D. Seiler; K. Wimmer

    2009-06-19

    Analysis of presolar grains in primitive meteorites has shown isotopic ratios largely characteristic of the conditions thought to prevail in various astrophysical environments. A possible indicator for a grain of ONe nova origin is a large 33S abundance: nucleosynthesis calculations predict as much as 150 times the solar abundance of 33S in the ejecta of nova explosions on massive ONe white dwarfs. This overproduction factor may, however, vary by factors of at least 0.01 - 3 because of uncertainties of several orders of magnitude in the 33S(p,gamma)34Cl reaction rate at nova peak temperatures (Tpeak ~ 0.1 - 0.4 GK). These uncertainties arise due to the lack of nuclear physics information for states within ~ 600 keV of the 33S+p threshold in 34Cl (Sp(34Cl) = 5143 keV). To better constrain this rate we have measured, for the first time, the 34S(3He,t)34Cl reaction over the region Ex(34Cl) = 4.9 - 6 MeV. We confirm previous states and find 15 new states in this energy region. New 33S(p,gamma)34Cl resonances at ER = 281(2), 301(2) and 342(2) keV may dominate this rate at relevant nova temperatures. Our results could affect predictions of sulphur isotopic ratios in nova ejecta (e.g., 32S/33S) that may be used as diagnostic tools for the nova paternity of grains.

  13. Full aperture backscatter station imager (FABSI) diagnostics system for far-field imaging of laser plasma instabilities on Nova

    SciTech Connect (OSTI)

    Wilke, M.D.; Fernandez, J.C.; Berggren, R.R.; Montgomery, D.; Faulkner, J.; Looney, L.; Jimerson, J.; Horton, R.F.

    1996-06-01

    In ICF, the understanding of laser plasma scattering processes is essential for laser target coupling and in controlling the symmetry of indirect drive implosions. The existing Nova Full Aperture Backscatter Station (FABS) has been useful in understanding laser plasma instabilities occurring in hohlraums by measuring the quantity, spectral distribution and near-field spatial distributions of Brillouin and more recently Raman backscatter. Equally important is an understanding of the farfield spatial intensity distribution which provides information on density, temperature and velocity gradient distributions, and which affect capsule implosion symmetry in hohlraums. Such information could potentially help in understanding processes such as filamentation and saturation mechanism. This paper describes a broad-band, color-corrected far-field imager and associated diagnostics capable of imaging the source of scattered light to better than 25 {micro}m resolution. The imager can either image Brillouin or Raman backscatter through the Nova beam 7 focusing lens or be used like a microscope to image side scatter from other beams.

  14. Quark-Novae in massive binaries : a model for double-humped, hydrogen-poor, superluminous Supernovae

    E-Print Network [OSTI]

    Ouyed, Rachid; Koning, Nico

    2015-01-01

    LSQ14bdq and SN 2006oz are super-luminous, hydrogen-poor, SNe with double-humped light curves. We show that a Quark-Nova (QN; explosive transition of the neutron star to a quark star) occurring in a massive binary, experiencing two Common Envelope (CE) phases, can quantitatively explain the light curves of LSQ14bdq and SN 2006oz. The more massive component (A) explodes first as a normal SN, yielding a Neutron Star which ejects the hydrogen envelope of the companion when the system enters its first CE phase. During the second CE phase, the NS spirals into and inflates the second He-rich CE. In the process it gains mass and triggers a Quark-Nova, outside of the CO core, leaving behind a Quark Star. The first hump in our model is the QN shock re-energizing the expanded He-rich CE. Subsequent merging of the Quark Star with the CO core of component B turns the Quark star to a Black Hole. The ensuing Black Hole accretion provides sufficient power for the second brighter and long lasting hump. Our model suggests a p...

  15. Insights into the evolution of symbiotic recurrent novae from radio synchrotron emission: V745 Scorpii and RS Ophiuchi

    E-Print Network [OSTI]

    Kantharia, N G; Roy, Nirupam; Anupama, G C; Ishwara-Chandra, C H; Chitale, A; Prabhu, T P; Banerjee, D P K; Ashok, N M

    2015-01-01

    We present observations at 610 MHz and 235 MHz using the Giant Metrewave Radio Telescope (GMRT) of the recurrent nova V745 Scorpii which recorded its last outburst on 6 February 2014. This is the second symbiotic recurrent nova whose light curve at GMRT frequencies has been followed in detail, the first being RS Ophiuchi in 2006. We fitted the 610 MHz light curve by a model of synchrotron emission from an expanding shell being modified by radiative transfer effects due to local absorbing gas consisting of a uniformly distributed and a clumpy component. Using our model parameters, we find that the emission at 235 MHz peaked around day 35 which is consistent with our GMRT observations. The two main results of our study are: (1) The radio emission at a given frequency is visible sooner after the outburst in successive outbursts of both V745 Scorpii and RS Ophiuchi. The earlier detection of radio emission is interpreted to be caused by decreasing foreground densities. (2) The clumpy material is located close to t...

  16. The October 1985 Long Outburst of U Geminorum: Revealing the Viscous Time Scale in Long Orbital Period Dwarf Novae

    E-Print Network [OSTI]

    John K. Cannizzo; Neil Gehrels; Janet A. Mattei

    2002-07-11

    We examine the AAVSO light curve of U Geminorum from 1908 to 2002, with particular focus on the October 1985 outburst. This outburst was longer than any other seen in U Gem by about a factor of 2, and appears to be unique among all dwarf nova outbursts seen in systems with orbital periods longer than 3 hr in that one can measure the decay time scale during the initial slow decay. This rate is ~26+-6 d/mag. Using estimates of the rate of accretion during outburst taken from Froning et al., one can show that ~1e24 g of gas was accreted onto the white dwarf during the outburst. When coupled with the viscous time inferred from the (short orbital period) SU UMa stars, the U Gem viscous time scale lends support to the standard model in which the decays in dwarf novae can either be viscous or thermal, with the ratio between them being roughly h/r where h is the vertical pressure scale height in the disk.

  17. A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption

    E-Print Network [OSTI]

    Darnley, M J; Steele, I A; Bode, M F; Ribeiro, V A R M; Rodríguez-Gil, P; Shafter, A W; Williams, S C; Baer, D; Hachisu, I; Hernanz, M; Hornoch, K; Hounsell, R; Kato, M; Kiyota, S; Ku?áková, H; Maehara, H; Ness, J -U; Piascik, A S; Sala, G; Skillen, I; Smith, R J; Wolf, M

    2015-01-01

    The Andromeda Galaxy recurrent nova M31N 2008-12a had been caught in eruption eight times. The inter-eruption period of M31N 2008-12a is ~1 year, making it the most rapidly recurring system known, and a strong single-degenerate Type Ia Supernova progenitor candidate. Following the 2013 eruption, a campaign was initiated to detect the predicted 2014 eruption and to then perform high cadence optical photometric and spectroscopic monitoring using ground-based telescopes, along with rapid UV and X-ray follow-up with the Swift satellite. Here we report the results of a high cadence multicolour optical monitoring campaign, the spectroscopic evolution, and the UV photometry. We also discuss tantalising evidence of a potentially related, vastly-extended, nebulosity. The 2014 eruption was discovered, before optical maximum, on October 2, 2014. We find that the optical properties of M31N 2008-12a evolve faster than all Galactic recurrent novae known, and all its eruptions show remarkable similarity both photometrically...

  18. Suzaku X-Ray Observation of the Dwarf Nova Z Camelopardalis at the Onset of an Optical Outburst

    E-Print Network [OSTI]

    Saitou, Kei; Ebisawa, Ken; Ishida, Manabu

    2012-01-01

    We present the result of a Suzaku X-ray spectroscopic observation of the dwarf nova Z Camelopardalis, which was conducted by chance at the onset of an optical outburst. We used the X-ray Imaging Spectrometer (a 38 ks exposure) and the Hard X-ray Detector (34 ks) to obtain a 0.35-40 keV spectrum simultaneously. Spectral characteristics suggest that the source was in the X-ray quiescent state despite being in the rising phase of an outburst in the optical band. The spectrum shows a clear signature of circumstellar absorption in excess of interstellar absorption and the reprocessed emission features of Fe fluorescence and Compton scattering. The extra absorption is explained due to partial coverage by either neutral or ionized matter. We found a spectral change during the observation, which is attributable only to the change in the circumstellar absorption. Such an X-ray spectral variation is reported for the first time in dwarf novae. We speculate that the variation in the circumstellar absorption is interprete...

  19. Discovery of $^{34g,m}$Cl$(p,\\gamma)^{35}$Ar resonances activated at classical nova temperatures

    E-Print Network [OSTI]

    Fry, C; Bishop, S; Brown, B A; Chen, A A; Faestermann, T; Hertenberger, R; Parikh, A; Pérez-Loureiro, D; Wirth, H -F; García, A; Ortez, R

    2015-01-01

    Background: The thermonuclear $^{34g,m}$Cl($p,\\gamma$)$^{35}$Ar reaction rates are unknown due to a lack of experimental nuclear physics data. Uncertainties in these rates translate to uncertainties in $^{34}$S production in models of classical novae on oxygen-neon white dwarfs. $^{34}$S abundances have the potential to aid in the classification of presolar grains. Purpose: Determine resonance energies for the $^{34g,m}$Cl($p,\\gamma$)$^{35}$Ar reactions within the region of astrophyical interest for classical novae to a precision of a few keV as an essential first step toward constraining their thermonuclear reaction rates. Method: $^{35}$Ar excited states were populated by the $^{36}$Ar($d,t$)$^{35}$Ar reaction at $E$(d)=22~MeV and reaction products were momentum analyzed by a high resolution quadrupole-dipole-dipole-dipole (Q3D) magnetic spectrograph. Results: Seventeen new $^{35}$Ar levels have been detected at a statistically significant level in the region $E_x\\approx$~5.9-6.7~MeV ($E_r$ \\textless~800~ k...

  20. A remarkable recurrent nova in M 31: The predicted 2014 outburst in X-rays with Swift

    E-Print Network [OSTI]

    Henze, M; Darnley, M J; Bode, M F; Williams, S C; Shafter, A W; Sala, G; Kato, M; Hachisu, I; Hernanz, M

    2015-01-01

    The M 31 nova M31N 2008-12a was recently found to be a recurrent nova (RN) with a recurrence time of about 1 year. This is by far the fastest recurrence time scale of any known RNe. Our optical monitoring programme detected the predicted 2014 outburst of M31N 2008-12a in early October. We immediately initiated an X-ray/UV monitoring campaign with Swift to study the multiwavelength evolution of the outburst. We monitored M31N 2008-12a with daily Swift observations for 20 days after discovery, covering the entire supersoft X-ray source (SSS) phase. We detected SSS emission around day six after outburst. The SSS state lasted for approximately two weeks until about day 19. M31N 2008-12a was a bright X-ray source with a high blackbody temperature. The X-ray properties of this outburst were very similar to the 2013 eruption. Combined X-ray spectra show a fast rise and decline of the effective blackbody temperature. The short-term X-ray light curve showed strong, aperiodic variability which decreased significantly a...

  1. Tough Stuff: A Look Back at NOVA's "Making Stuff" Mini-Series

    Broader source: Energy.gov [DOE]

    Learn more about the Department's work with material science, including imitating the structure of mother of pearl to create the toughest ceramic ever produced and developing a new type of damage-tolerant metallic glass that's stronger and tougher than steel.

  2. Not. Astron. doi:10.1111/j.13652966.2005.09664.x An Xray emissionline spectrum of Nova V382 Velorum 1999

    E-Print Network [OSTI]

    Ness, Jan-Uwe

    X­ray grating spectrum Classical Nova V382 (1999), obtained with Low Energy Transmission Grating), of cataclysmic variables (CVs), thought to be thermonuclear explosions induced on surface of white dwarfs of hydrogen­rich fuel causes thermonuclear runaway (TNR). tensive modelling of been carried past Starrfield

  3. Photometric study of southern SU UMa-type dwarf novae and candidates -- III: NSV 10934, MM Sco, AB Nor, CAL 86

    E-Print Network [OSTI]

    T. Kato; P. Nelson; C. Stockdale; B. Monard; T. Richards; R. Stubbings; H. Yamaoka; B. Heathcote; R. Santallo

    2003-10-01

    We photometrically observed four southern dwarf novae in outburst (NSV 10934, MM Sco, AB Nor and CAL 86). NSV 10934 was confirmed to be an SU UMa-type dwarf nova with a mean superhump period of 0.07478(1) d. This star also showed transient appearance of quasi-periodic oscillations (QPOs) during the final growing stage of the superhumps. Combined with the recent theoretical interpretation and with the rather unusual rapid terminal fading of normal outbursts, NSV 10934 may be a candidate intermediate polar showing SU UMa-type properties. The mean superhump periods of MM Sco and AB Nor were determined to be 0.06136(4) d and 0.08438(2) d, respectively. We suggest that AB Nor belongs to a rather rare class of long-period SU UMa-type dwarf novae with low mass-transfer rates. We also observed an outburst of the suspected SU UMa-type dwarf nova CAL 86. We identified this outburst as a normal outburst and determined the mean decline rate of 1.1 mag/d.

  4. FAR-ULTRAVIOLET SPECTROSCOPY OF THE NOVA-LIKE VARIABLE KQ MONOCEROTIS: A NEW SW SEXTANTIS STAR?

    SciTech Connect (OSTI)

    Wolfe, Aaron; Sion, Edward M.; Bond, Howard E. E-mail: edward.sion@villanova.edu

    2013-06-01

    New optical spectra obtained with the SMARTS 1.5 m telescope and archival International Ultraviolet Explorer (IUE) far-ultraviolet (FUV) spectra of the nova-like variable KQ Mon are discussed. The optical spectra reveal Balmer lines in absorption as well as He I absorption superposed on a blue continuum. The 2011 optical spectrum is similar to the KPNO 2.1 m IIDS spectrum we obtained 33 years earlier except that the Balmer and He I absorption is stronger in 2011. Far-ultraviolet IUE spectra reveal deep absorption lines due to C II, Si III, Si IV, C IV, and He II, but no P Cygni profiles indicative of wind outflow. We present the results of the first synthetic spectral analysis of the IUE archival spectra of KQ Mon with realistic optically thick, steady-state, viscous accretion-disk models with vertical structure and high-gravity photosphere models. We find that the photosphere of the white dwarf (WD) contributes very little FUV flux to the spectrum and is overwhelmed by the accretion light of a steady disk. Disk models corresponding to a WD mass of {approx}0.6 M {sub Sun }, with an accretion rate of order 10{sup -9} M {sub Sun} yr{sup -1} and disk inclinations between 60 Degree-Sign and 75 Degree-Sign , yield distances from the normalization in the range of 144-165 pc. KQ Mon is discussed with respect to other nova-like variables. Its spectroscopic similarity to the FUV spectra of three definite SW Sex stars suggests that it is likely a member of the SW Sex class and lends support to the possibility that the WD is magnetic.

  5. Torus through Integrated Data Analysis Mark Nornberg Matthew Galante (Nova Photonics)

    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 AdministrationRobust,Field-effectWorking With U.S.Week DayDr.Theories81 toDepartment ofTopo Blue Gene/Q VersusZ

  6. XMM-NEWTON X-RAY AND ULTRAVIOLET OBSERVATIONS OF THE FAST NOVA V2491 Cyg DURING THE SUPERSOFT SOURCE PHASE

    SciTech Connect (OSTI)

    Ness, J.-U. [XMM-Newton Science Operations Centre, ESA, Madrid (Spain); Osborne, J. P.; Page, K. L.; Beardmore, A. P. [Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH (United Kingdom); Dobrotka, A. [Department of Physics, Institute of Materials Science, Faculty of Materials Science and Technology, Slovak University of Technology in Bratislava, 91724 Trnava (Slovakia); Drake, J. J. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Pinto, C.; Detmers, R. G. [SRON Netherlands Institute for Space Research, 3584 CA Utrecht (Netherlands); Schwarz, G. [American Astronomical Society, Washington, DC 20009-1231 (United States); Bode, M. F. [Astrophysics Research Institute, Liverpool John Moores University, Birkenhead CH41 1LD (United Kingdom); Starrfield, S. [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 (United States); Hernanz, M. [Institut de Ciencies de l'Espai (CSIC-IEEC), Campus UAB, Facultat de Ciencies, 08193 Bellaterra (Barcelona) (Spain); Sala, G. [Departament Fisica i Enginyeria Nuclear, EUETIB (UPC-IEEC), 08036 Barcelona (Spain); Krautter, J. [Landessternwarte Koenigstuhl, Universitaet Heidelberg, D-69117 Heidelberg (Germany); Woodward, C. E. [Department of Astronomy, University of Minnesota, Minneapolis, MN 55455 (United States)

    2011-05-20

    Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2 minutes after an extended factor of three decline lasting {approx}3 hr, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves of the novae V4743 Sgr and RS Oph, as it occurred on the same timescale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for four intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of O I and N I are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blueshifts indicating an expansion velocity of 3000-3400 km s{sup -1}, which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743 Sgr and the symbiotic recurrent nova RS Oph are presented. The SSS spectrum of V4743 Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RS Oph are as narrow as in V2491 Cyg, but they are less blueshifted. A remarkable similarity in the continua of V2491 Cyg and RS Oph is found. The only differences are smaller line shifts and additional emission lines in RS Oph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05 A, 29.45 A, and 30.0 A. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required.

  7. XMM-NEWTON OBSERVATIONS OF THE DWARF NOVA RU Peg IN QUIESCENCE: PROBE OF THE BOUNDARY LAYER

    SciTech Connect (OSTI)

    Balman, Soelen [Department of Physics, Middle East Technical University, Ankara (Turkey); Godon, Patrick; Sion, Edward M. [Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States); Ness, Jan-Uwe [XMM-Newton Science Operations Centre, European Space Agency (ESA/ESAC), E-28691 Villanueva de la Canada, Madrid (Spain); Schlegel, Eric [Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, TX 78249 (United States); Barrett, Paul E. [United States Naval Observatory, Washington, DC 20392 (United States); Szkody, Paula, E-mail: solen@astroa.physics.metu.edu.tr, E-mail: patrick.godon@villanova.edu, E-mail: edward.sion@villanova.edu, E-mail: juness@sciops.esa.int, E-mail: eric.schlegel@utsa.edu, E-mail: barrett.paul@usno.navy.mil, E-mail: szkody@astro.washington.edu [Astronomy Department, University of Seattle, Seattle, WA 98195 (United States)

    2011-11-10

    We present an analysis of X-ray and UV data obtained with the XMM-Newton Observatory of the long-period dwarf nova RU Peg. RU Peg contains a massive white dwarf (WD), possibly the hottest WD in a dwarf nova (DN), it has a low inclination, thus optimally exposing its X-ray emitting boundary layer (BL), and has an excellent trigonometric parallax distance. We modeled the X-ray data using XSPEC assuming a multi-temperature plasma emission model built from the MEKAL code (i.e., CEVMKL). We obtained a maximum temperature of 31.7 keV, based on the European Photon Imaging Camera MOS1, 2 and pn data, indicating that RU Peg has an X-ray spectrum harder than most DNe, except U Gem. This result is consistent with and indirectly confirms the large mass of the WD in RU Peg. The X-ray luminosity we computed corresponds to a BL luminosity for a mass accretion rate of 2 Multiplication-Sign 10{sup -11} M{sub sun} yr{sup -1} (assuming M{sub wd} = 1.3 M{sub sun}), in agreement with the expected quiescent accretion rate. The modeling of the O VIII emission line at 19 A as observed by the Reflection Grating Spectrometer implies a projected stellar rotational velocity v{sub rot}sin i = 695 km s{sup -1}, i.e., the line is emitted from material rotating at {approx}936-1245 km s{sup -1} (i {approx} 34 Degree-Sign -48 Degree-Sign) or about 1/6 of the Keplerian speed; this velocity is much larger than the rotation speed of the WD inferred from the Far Ultraviolet Spectroscopic Explorer spectrum. Cross-correletion analysis yielded an undelayed (time lag {approx} 0) component and a delayed component of 116 {+-} 17 s where the X-ray variations/fluctuations lagged the UV variations. This indicates that the UV fluctuations in the inner disk are propagated into the X-ray emitting region in about 116 s. The undelayed component may be related to irradiation effects.

  8. Classical-Nova Contribution to the Milky Way's $^{26}$Al Abundance: Exit Channel of the Key $^{25}$Al($p,?$)$^{26}$Si Resonance

    E-Print Network [OSTI]

    M. B. Bennett; C. Wrede; K. A. Chipps; J. José; S. N. Liddick; M. Santia; A. Bowe; A. A. Chen; N. Cooper; D. Irvine; E. McNeice; F. Montes; F. Naqvi; R. Ortez; S. D. Pain; J. Pereira; C. Prokop; J. Quaglia; S. J. Quinn; S. B. Schwartz; S. Shanab; A. Simon; A. Spyrou; E. Thiagalingam

    2013-12-12

    Classical novae are expected to contribute to the 1809-keV Galactic $\\gamma$-ray emission by producing its precursor $^{26}$Al, but the yield depends on the thermonuclear rate of the unmeasured $^{25}$Al($p,\\gamma$)$^{26}$Si reaction. Using the $\\beta$ decay of $^{26}$P to populate the key $J^{\\pi}=3^+$ resonance in this reaction, we report the first evidence for the observation of its exit channel via a $1741.6 \\pm 0.6 (\\textrm{stat}) \\pm 0.3 (\\textrm{syst})$ keV primary $\\gamma$ ray, where the uncertainties are statistical and systematic, respectively. By combining the measured $\\gamma$-ray energy and intensity with other experimental data on $^{26}$Si, we find the center-of-mass energy and strength of the resonance to be $E_r = 414.9 \\pm 0.6(\\textrm{stat}) \\pm 0.3 (\\textrm{syst}) \\pm 0.6(\\textrm{lit.})$ keV and $\\omega\\gamma = 23 \\pm 6 (\\textrm{stat})^{+11}_{-10}(\\textrm{lit.})$ meV, respectively, where the last uncertainties are from adopted literature data. We use hydrodynamic nova simulations to model $^{26}$Al production showing that these measurements effectively eliminate the dominant experimental nuclear-physics uncertainty and we estimate that novae may contribute up to 30% of the Galactic $^{26}$Al.

  9. Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VII: The Seventh Year (2014-2015)

    E-Print Network [OSTI]

    Kato, Taichi; Dubovsky, Pavol A; Kudzej, Igor; Monard, Berto; Miller, Ian; Itoh, Hiroshi; Kiyota, Seiichiro; Masumoto, Kazunari; Fukushima, Daiki; Kinoshita, Hiroki; Maeda, Kazuki; Mikami, Jyunya; Matsuda, Risa; Kojiguchi, Naoto; Kawabata, Miho; Takenaka, Megumi; Matsumoto, Katsura; de Miguel, Enrique; Maeda, Yutaka; Ohshima, Tomohito; Isogai, Keisuke; Pickard, Roger D; Henden, Arne; Kafka, Stella; Akazawa, Hidehiko; Otani, Noritoshi; Ishibashi, Sakiko; Ogi, Minako; Tanabe, Kenji; Imamura, Kazuyoshi; Stein, William; Kasai, Kiyoshi; Vanmunster, Tonny; Starr, Peter; Pavlenko, Elena P; Antonyuk, Oksana I; Antonyuk, Kirill A; Sosnovskij, Aleksei A; Pit, Nikolaj V; Babina, Julia V; Sklyanov, Aleksandr; Novak, Rudolf; Oksanen, Arto; Dvorak, Shawn; Michel, Raul; Masi, Gianluca; Littlefield, Colin; Ulowetz, Joseph; Shugarov, Sergey Yu; Golysheva, Polina Yu; Chochol, Drahomir; Krushevska, Viktoriia; Ruiz, Javier; Tordai, Tamas; Morelle, Etienne; Sabo, Richard; Maehara, Hiroyuki; Richmond, Michael; Katysheva, Natalia; Hirosawa, Kenji; Goff, William N; Dubois, Franky; Logie, Ludwig; Rau, Steve; Voloshina, Irina B; Andreev, Maksim V; Shiokawa, Kazuhiko; Neustroev, Vitaly V; Sjoberg, George; Zharikov, Sergey; James, Nick; Bolt, Greg; Crawford, Tim; Buczynski, Denis; Cook, Lewis M; Kochanek, Christopher S; Shappee, Benjamin; Stanek, Krzysztof Z; Prieto, Jose L; Denisenko, Denis; Nishimura, Hideo; Mukai, Masaru; Kaneko, Shizuo; Ueda, Seiji; Stubbings, Rod; Moriyama, Masayuki; Schmeer, Patrick; Muyllaert, Eddy; Shears, Jeremy; Modic, Robert J; Paxson, Kevin B

    2015-01-01

    Continuing the project described by Kato et al. (2009, arXiv:0905.1757), we collected times of superhump maxima for 102 SU UMa-type dwarf novae observed mainly during the 2014-2015 season and characterized these objects. Our project has greatly improved the statistics of the distribution of orbital periods, which is a good approximation of the distribution of cataclysmic variables at the terminal evolutionary stage, and confirmed the presence of a period minimum at a period of 0.053 d and a period spike just above this period. The number density monotonically decreased toward the longer period and there was no strong indication of a period gap. We detected possible negative superhumps in Z Cha. It is possible that normal outbursts are also suppressed by the presence of a disk tilt in this system. There was no indication of enhanced orbital humps just preceding the superoutburst, and this result favors the thermal-tidal disk instability as the origin of superoutbursts. We detected superhumps in three AM CVn-ty...

  10. X-ray Eclipse Diagnosis of the Evolving Mass Loss in the Recurrent Nova U Scorpii 2010

    E-Print Network [OSTI]

    Takei, D; Tsujimoto, M; Ness, J -U; Osborne, J P; Starrfield, S; Kitamoto, S

    2013-01-01

    We report the Suzaku detection of the earliest X-ray eclipse seen in the recurrent nova U Scorpii 2010. A target-of-opportunity observation 15 days after the outburst found a 27+/-5% dimming in the 0.2-1.0 keV energy band at the predicted center of an eclipse. In comparison with the X-ray eclipse depths seen at two later epochs by XMM-Newton, the source region shrank by about 10-20% between days 15 and 35 after the outburst. The X-ray eclipses appear to be deeper than or similar to contemporaneous optical eclipses, suggesting the X-ray and optical source region extents are comparable on day 15. We raise the possibility of the energy dependency in the photon escape regions, and that this would be a result of the supersoft X-ray opacity being higher than the Thomson scattering optical opacity at the photosphere due to bound-free transitions in abundant metals that are not fully ionized. Assuming a spherically symmetric explosion model, we constrain the mass-loss rate as a function of time. For a ratio of actual...

  11. X-RAY ECLIPSE DIAGNOSIS OF THE EVOLVING MASS LOSS IN THE RECURRENT NOVA U SCORPII 2010

    SciTech Connect (OSTI)

    Takei, D.; Drake, J. J. [Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States); Tsujimoto, M. [Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, 3-1-1 Yoshino-dai, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan); Ness, J.-U. [European Space Agency, XMM-Newton Observatory SOC, SRE-OAX, Apartado 78, E-28691 Villanueva de la Canada, Madrid (Spain); Osborne, J. P. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Starrfield, S. [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 (United States); Kitamoto, S., E-mail: dtakei@head.cfa.harvard.edu [Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo 171-8501 (Japan)

    2013-05-20

    We report the Suzaku detection of the earliest X-ray eclipse seen in the recurrent nova U Scorpii 2010. A target-of-opportunity observation 15 days after the outburst found a 27% {+-} 5% dimming in the 0.2-1.0 keV energy band at the predicted center of an eclipse. In comparison with the X-ray eclipse depths seen at two later epochs by XMM-Newton, the source region shrank by about 10%-20% between days 15 and 35 after the outburst. The X-ray eclipses appear to be deeper than or similar to contemporaneous optical eclipses, suggesting the X-ray and optical source region extents are comparable on day 15. We raise the possibility of the energy dependency in the photon escape regions, and that this would be a result of the supersoft X-ray opacity being higher than the Thomson scattering opacity at the photosphere due to bound-free transitions in abundant metals that are not fully ionized. Assuming a spherically symmetric model, we constrain the mass-loss rate as a function of time. For a ratio of actual to Thomson opacity of 10-100 in supersoft X-rays, we find an ejecta mass of about 10{sup -7}-10{sup -6} M{sub Sun }.

  12. Swift detection of the super-swift switch-on of the super-soft phase in nova V745 Sco (2014)

    E-Print Network [OSTI]

    Page, K L; Kuin, N P M; Henze, M; Walter, F M; Beardmore, A P; Bode, M F; Darnley, M J; Delgado, L; Drake, J J; Hernanz, M; Mukai, K; Nelson, T; Ness, J -U; Schwarz, G J; Shore, S N; Starrfield, S; Woodward, C E

    2015-01-01

    V745 Sco is a recurrent nova, with the most recent eruption occurring in February 2014. V745 Sco was first observed by Swift a mere 3.7 hr after the announcement of the optical discovery, with the super-soft X-ray emission being detected around four days later and lasting for only ~two days, making it both the fastest follow-up of a nova by Swift and the earliest switch-on of super-soft emission yet detected. Such an early switch-on time suggests a combination of a very high velocity outflow and low ejected mass and, together with the high effective temperature reached by the super-soft emission, a high mass white dwarf (>1.3 M_sun). The X-ray spectral evolution was followed from an early epoch where shocked emission was evident, through the entirety of the super-soft phase, showing evolving column density, emission lines, absorption edges and thermal continuum temperature. UV grism data were also obtained throughout the super-soft interval, with the spectra showing mainly emission lines from lower ionization...

  13. Extraordinary luminous soft X-ray transient MAXI J0158–744 as an ignition of a nova on a very massive O-Ne white dwarf

    SciTech Connect (OSTI)

    Morii, M.; Serino, M.; Mihara, T.; Sugizaki, M.; Tomida, H.; Kimura, M.; Nakahira, S.; Suwa, F.; Negoro, H.; Kennea, J. A.; Pritchard, T.; Page, K. L.; Osborne, J. P.; Curran, P. A.; Walter, F. M.; Kuin, N. P. M.; Hiroi, K.; Usui, R.; Kawai, N.; Gehrels, N.; and others

    2013-12-20

    We present the observation of an extraordinary luminous soft X-ray transient, MAXI J0158–744, by the Monitor of All-sky X-ray Image (MAXI) on 2011 November 11. This transient is characterized by a soft X-ray spectrum, a short duration (1.3 × 10{sup 3} s < ?T{sub d} < 1.10 × 10{sup 4} s), a rapid rise (<5.5 × 10{sup 3} s), and a huge peak luminosity of 2 × 10{sup 40} erg s{sup –1} in 0.7-7.0 keV band. With Swift observations and optical spectroscopy from the Small and Moderate Aperture Research Telescope System, we confirmed that the transient is a nova explosion, on a white dwarf in a binary with a Be star, located near the Small Magellanic Cloud. An early turn-on of the super-soft X-ray source (SSS) phase (<0.44 days), the short SSS phase duration of about one month, and a 0.92 keV neon emission line found in the third MAXI scan, 1296 s after the first detection, suggest that the explosion involves a small amount of ejecta and is produced on an unusually massive O-Ne white dwarf close to, or possibly over, the Chandrasekhar limit. We propose that the huge luminosity detected with MAXI was due to the fireball phase, a direct manifestation of the ignition of the thermonuclear runaway process in a nova explosion.

  14. Biogeography of Marine Algae

    E-Print Network [OSTI]

    Biogeography of Marine Algae David J Garbary, St Francis Xavier University, Antigonish, Nova Scotia and vicariance in establishing distributions and as factors associated with speciation. Since eukaryotic algae. There are many species that are virtually cosmopolitan (e.g. the green alga Enteromorpha intestinalis, the red

  15. North American Journal of Fisheries Management 22:770784, 2002 Copyright by the American Fisheries Society 2002

    E-Print Network [OSTI]

    Myers, Ransom A.

    Hydroelectric Generating Station, Nova Scotia A. JAMIE F. GIBSON* Acadia Centre for Estuarine Research, Post structures such as the intake pipes at cooling water plants or the turbine intakes at hydroelectric abundance, behavior, and rates of passage at hydroelectric stations vary considerably in re- sponse

  16. J. Paleont., 83(1), 2009, pp. 140146 Copyright 2009, The Paleontological Society

    E-Print Network [OSTI]

    Martino, Ronald L.

    from Ohio, Pennsylvania, Illinois, and Nova Scotia. Only four Arthropleura trackway sites have been.The track- ways were found in the lower Conemaugh Formation of Ken- tucky, equivalent to the Glenshaw Formation of the Conemaugh Group in neighboring West Virginia. The Glenshaw Formation consists predominantly

  17. A Computationally Stable Approach to Gaussian Process Interpolation of Deterministic

    E-Print Network [OSTI]

    Ranjan, Pritam

    extractable tidal power as a function of the turbine locations in the Bay of Fundy, Nova Scotia, Canada. The deter- ministic computer simulator for the tidal power model is a nu- merical solver of a complex system of partial differential equa- tions, and we accept the simulator as a valid representation of the tidal power

  18. Interannual Changes in Seasonal Ground Freezing and Near-surface Heat Flow Beneath Bottom-fast Ice in the Near-shore Zone, Mackenzie Delta, NWT, Canada

    E-Print Network [OSTI]

    Moorman, Brian

    Interannual Changes in Seasonal Ground Freezing and Near-surface Heat Flow Beneath Bottom-fast Ice Resources Canada, Dartmouth, Nova Scotia, Canada ABSTRACT Interannual changes in seasonal ground freezing. KEY WORDS: seasonal ground freezing; permafrost; bottom-fast ice; Mackenzie Delta INTRODUCTION Arctic

  19. Some electric myths Larry Hughes

    E-Print Network [OSTI]

    Hughes, Larry

    industrial demand (460 GWh), there has also been a significant increase in residential electricity demand in residential electricity demand is the result of the increased use of electricity for space heating since and Nova Scotia's demand for electricity, both of which are based, in part, upon the arguments made when

  20. Meeting NSPI's 2010 SO2 emission reduction cap Larry Hughes, Mandeep Dhaliwal, and Nikita Sheth

    E-Print Network [OSTI]

    Hughes, Larry

    is the principal fuel used by NSPI (see Table 2). Table 2: NSPI's generation by fuel type (MWh) (Toner, 2006) Coal of the highest in the country is Nova Scotia Power's reliance on coal for electrical generation. Given NSPI into the industrial and utility sector, and the continued use of low-sulphur coal. With the Sable Offshore Energy

  1. Migration cues and timing in leatherback sea turtles

    E-Print Network [OSTI]

    Myers, Ransom A.

    Migration cues and timing in leatherback sea turtles Scott A. Sherrill-Mix, Michael C. James, Nova Scotia, Canada B3H 4J1 Atlantic leatherback sea turtles migrate annually from foraging grounds off's proportional hazards model, we investigated the individual timing of the southward migrations of 27 turtles

  2. JSS Journal of Statistical Software March 2015, Volume 64, Issue 12. http://www.jstatsoft.org/

    E-Print Network [OSTI]

    Ranjan, Pritam

    .e., for emulating the tidal kinetic energy model for the Bay of Fundy, Nova Scotia, Canada. GPfit is free software and distributed under the General Public License and available from the Comprehensive R Archive Network. Keywords), dynamics of dark energy and dark matter in cosmological studies (Arbey 2006), and the tidal kinetic energy

  3. This article was downloaded by: [Universita Studi la Sapienza] On: 22 May 2015, At: 07:37

    E-Print Network [OSTI]

    Sciortino, Francesco

    : Taylor & Francis Informa Ltd Registered in England and Wales Registered Number: 1072954 Registered office for authors and subscription information: http://www.tandfonline.com/loi/tmph20 Phase diagram of the ST2 model of Physics, St. Francis Xavier University, Nova Scotia, Canada c Dipartimento di Fisica, Università di Roma

  4. Early Jurassic eolian dune field, Pomperaug basin, Connecticut and related synrift deposits

    E-Print Network [OSTI]

    LeTourneau, Peter M.

    Early Jurassic eolian dune field, Pomperaug basin, Connecticut and related synrift deposits eolian sandstone in the Pomperaug basin, Connecticut is noteworthy because it is the most significant from the Hartford (Connecticut, USA), Fundy (Nova Scotia, Canada), and Argana (Morocco) basins. Using

  5. E-Voting in Brazil -The Risks to Democracy Jos Rodrigues-Filho, Cynthia J. Alexander, and Luciano C. Batista

    E-Print Network [OSTI]

    Matwin, Stan

    - 85 - E-Voting in Brazil - The Risks to Democracy José Rodrigues-Filho, Cynthia J. Alexander, and Luciano C. Batista Federal University of Paraiba, Paraiba, Brazil and Acadia University, Nova Scotia be implemented - then the implications for democracy should be considered. Brazil's introduction of e

  6. Optimization of duplex real-time PCR with melting-curve analysis for detecting the microsporidian

    E-Print Network [OSTI]

    Shutler, Dave

    and 18 pooled samples of 15 workers) collected in Nova Scotia, Prince Edward Island, and Newfoundland´chantillons collectifs de 15 ouvrie`res) re´colte´s en Nouvelle-E´ cosse, a` l'I^le-du-Prince-E´ douard Received 13

  7. DALHOUSIE UNIVERSITY LIBRARIES Collections Strategy Librarian

    E-Print Network [OSTI]

    Brownstone, Rob

    for acquiring, preserving and sharing knowledge. As academic resources become format-agnostic and increasingly, Science, Management, and Computer Science), the W.K. Kellogg Health Sciences Library (Medicine, Dentistry of Nova Scotia academic libraries sharing a common library management system (Ex Libris Aleph 500

  8. US Department

    Energy Savers [EERE]

    personnel management and security programs, administrative support services, and information technology programs. U.S. Department of Energy, Office of Inspector General...

  9. DEPARTMENT OF DEPARTMENT OF BIOLOGY

    E-Print Network [OSTI]

    Turc, Catalin

    Masters of Science Degree Plan A: Thesis DEPARTMENT OF BIOLOGY CASE WESTERN RESERVE UNIVERSITY #12;DEPARTMENT OF BIOLOGY Masters of Science Degree (Plan A) Thesis The Plan A Master of Science Degree in Biology is a thesis,graduate degree program.The purpose of the program is to provide advanced exposure

  10. DEPARTMENT OF CHEMISTRY DEPARTMENT OF CHEMISTRY

    E-Print Network [OSTI]

    Lennard, William N.

    i DEPARTMENT OF CHEMISTRY HANDBOOK 2008-2009 DEPARTMENT OF CHEMISTRY HANDBOOK 2014-2015 Revised TABLE OF CONTENTS I. WELCOME TO THE DEPARTMENT OF CHEMISTRY AND WESTERN UNIVERSITY... 1 1. MESSAGE FROM

  11. US Department

    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.Laclede GasEfficiency|Feed| DepartmentOF CALIFORNIADepartment ofUS Department

  12. "Managing Department Climate Change"

    E-Print Network [OSTI]

    Sheridan, Jennifer

    "Managing Department Climate Change" #12;Presenters · Ronda Callister Professor, Department Department Climate? · Assesment is essential for determining strategies for initiating change · In a research climate · Each panelist will describe an intervention designed to improve department climate ­ Ronda

  13. Light Curves of Core-Collapse Supernovae with Substantial Mass Loss using the New Open-Source SuperNova Explosion Code (SNEC)

    E-Print Network [OSTI]

    Morozova, V; Renzo, M; Ott, C D; Clausen, D; Couch, S M; Ellis, J; Roberts, L F

    2015-01-01

    We present the SuperNova Explosion Code SNEC, an open-source Lagrangian code for the hydrodynamics and equilibrium-diffusion radiation transport in the expanding envelopes of supernovae. Given a model of a progenitor star, an explosion energy, and an amount and distribution of radioactive nickel, SNEC generates the bolometric light curve, as well as the light curves in different wavelength bands assuming black body emission. As a first application of SNEC, we consider the explosions of a grid of 15 Msun (at zero-age main sequence) stars whose hydrogen envelopes are stripped to different extents and at different points in their evolution. The resulting light curves exhibit plateaus with durations of ~20-100 days if >~1.5-2 Msun of hydrogen-rich material is left and no plateau if less hydrogen-rich material is left. The shorter plateau lengths are unlike the Type IIP supernova light curves typically observed in nature. This suggests that, at least for zero-age main sequence masses <~ 20 Msun, hydrogen mass l...

  14. Multi-wavelength Light Curve Model of the One-year Recurrence Period Nova M31N 2008-12a

    E-Print Network [OSTI]

    Kato, Mariko; Hachisu, Izumi

    2015-01-01

    We present a theoretical light curve model of the recurrent nova M31N 2008-12a, the current record holder for the shortest recurrence period (1 yr). We combined interior structures calculated using a Henyey-type evolution code with optically thick wind solutions of hydrogen-rich envelopes, which give the proper mass-loss rates, photospheric temperatures, and luminosities. The light curve model is calculated for a 1.38 M_sun white dwarf (WD) with an accretion rate of 1.6 \\times 10^{-7} M_sun yr^{-1}. This model shows a very high effective temperature (log T_ph (K) \\geq 4.97) and a very small wind mass-loss rate (\\dot M_wind \\leq 9.3 \\times 10^{-6} M_sun yr^{-1}) even at the maximum expansion of the photosphere. These properties are consistent with the faint optical peak of M31N 2008-12a because the brightness of the free-free emission is proportional to the square of the mass-loss rate. The model well reproduces the short supersoft X-ray turn-on time of 6 days and turnoff time of 18 days after the outburst. Th...

  15. DEPARTMENT CODE Department of Computer Science

    E-Print Network [OSTI]

    DEPARTMENT CODE Department of Computer Science College of Natural Sciences Colorado State and Amendment of this Code 19 #12;1 MISSION AND OBJECTIVES 3 Preamble This Code of the Department of Computer Science1 is a manual of operation that describes the functioning of the Department by codifying policy

  16. Working with Department Enhancing Department Climate

    E-Print Network [OSTI]

    Sheridan, Jennifer

    Working with Department Chairs: Enhancing Department Climate #12;The Department Climate Survey 21% Graduate Student 232 21% No response/blank 31 3% Total 1121 100% #12;Findings: Overall Department Climate Score Mean overall climate score = 3.72 (scale of 1-5) Rating N % Very negative (1) 30 2.7% Negative (2

  17. QUARK-NOVAE IN LOW-MASS X-RAY BINARIES. II. APPLICATION TO G87-7 AND TO GRB 110328A

    SciTech Connect (OSTI)

    Ouyed, Rachid; Staff, Jan; Jaikumar, Prashanth

    2011-12-20

    We propose a simple model explaining two outstanding astrophysical problems related to compact objects: (1) that of stars such as G87-7 (alias EG 50) that constitute a class of relatively low-mass white dwarfs (WDs) which nevertheless fall away from the C/O composition and (2) that of GRB 110328A/Swift J164449.3+57345 which showed spectacularly long-lived strong X-ray flaring, posing a challenge to standard gamma-ray burst models. We argue that both these observations may have an explanation within the unified framework of a quark-nova (QN) occurring in a low-mass X-ray binary (LMXB; neutron star (NS)-WD). For LMXBs, where the binary separation is sufficiently tight, ejecta from the exploding NS triggers nuclear burning in the WD on impact, possibly leading to Fe-rich composition compact WDs with mass 0.43 M{sub Sun} < M{sub WD} < 0.72 M{sub Sun }, reminiscent of G87-7. Our results rely on the assumption, which ultimately needs to be tested by hydrodynamic and nucleosynthesis simulations, that under certain circumstances the WD can avoid the thermonuclear runaway. For heavier WDs (i.e., M{sub WD} > 0.72 M{sub Sun }) experiencing the QN shock, degeneracy will not be lifted when carbon burning begins, and a sub-Chandrasekhar Type Ia supernova may result in our model. Under slightly different conditions and for pure He WDs (i.e., M{sub WD} < 0.43 M{sub Sun }), the WD is ablated and its ashes raining down on the quark star (QS) leads to accretion-driven X-ray luminosity with energetics and duration reminiscent of GRB 110328A. We predict additional flaring activity toward the end of the accretion phase if the QS turns into a black hole.

  18. A self-consistent MoD-WM/MM structural refinement method: characterization of hydrogen bonding in the orytricha nova G-1uar

    SciTech Connect (OSTI)

    Batista, Enrique R [Los Alamos National Laboratory; Newcomer, Micharel B [YALE UNIV; Raggin, Christina M [YALE UNIV; Gascon, Jose A [YALE UNIV; Loria, J Patrick [YALE UNIV; Batista, Victor S [YALE UNIV

    2008-01-01

    This paper generalizes the MoD-QM/MM hybrid method, developed for ab initio computations of protein electrostatic potentials [Gasc6n, l.A.; Leung, S.S.F.; Batista, E.R.; Batista, V.S. J. Chem. Theory Comput. 2006,2, 175-186], as a practical algorithm for structural refinement of extended systems. The computational protocol involves a space-domain decomposition scheme for the formal fragmentation of extended systems into smaller, partially overlapping, molecular domains and the iterative self-consistent energy minimization of the constituent domains by relaxation of their geometry and electronic structure. The method accounts for mutual polarization of the molecular domains, modeled as Quantum-Mechanical (QM) layers embedded in the otherwise classical Molecular-Mechanics (MM) environment according to QM/MM hybrid methods. The method is applied to the description of benchmark models systems that allow for direct comparisons with full QM calculations, and subsequently applied to the structural characterization of the DNA Oxytricha nova Guanine quadruplex (G4). The resulting MoD-QM/MM structural model of the DNA G4 is compared to recently reported highresolution X-ray diffraction and NMR models, and partially validated by direct comparisons between {sup 1}H NMR chemical shifts that are highly sensitive to hydrogen-bonding and stacking interactions and the corresponding theoretical values obtained at the density functional theory DFT QM/MM (BH&H/6-31 G*:Amber) level in conjunction with the gauge independent atomic orbital (GIAO) method for the ab initio self consistent-field (SCF) calculation of NMR chemical shifts.

  19. Department Chairs in PSOM Departments Department Chair Phone Email

    E-Print Network [OSTI]

    Sharp, Kim

    Department Chairs in PSOM Departments Department Chair Phone Email Anesthesiology and Critical Care@mail.med.upenn.edu Cancer Biology Lewis Chodosh, MD, PhD 898-1321 chodosh@mail.med.upenn.edu Cell & Developmental Biology@mail.med.upenn.edu Radiation Oncology James M. Metz, MD (Interim) 662-2428 metz@uphs.upenn.edu Radiology Mitchell D. Schnall

  20. Department Head Resource Portal

    E-Print Network [OSTI]

    Salvaggio, Carl

    1 Department Head Resource Portal CREATING DEPARTMENT GOALS A goal is a condition we envision;2 Department Head Resource Portal NO DO YOU HAVE IT? YES ffff Achieve Preserve Avoid Eliminate NO DO YOU HAVE

  1. COMPUTER ENGINEERING EECS Department

    E-Print Network [OSTI]

    COMPUTER ENGINEERING EECS Department The Electrical Engineering and Computer Science (EECS) Department at WSU offers undergraduate degrees in electrical engineering, computer engineering and computer science. The EECS Department offers Master of Science degrees in computer science, electrical engineering

  2. Department of Engineering.

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    Department of Civil & Structural Engineering. Vibration based Structural Health Monitoring James views of the same spectrum Department of Civil & Structural Engineering. Structural health monitoring of Sheffield, United Kingdom Department of Civil & Structural Engineering. HEALTH and PERFORMANCE are different

  3. ELECTRICAL ENGINEERING EECS Department

    E-Print Network [OSTI]

    ELECTRICAL ENGINEERING EECS Department The Electrical Engineering and Computer Science (EECS) Department at WSU offers undergraduate degrees in electrical engineering, computer engineering and computer science. The EECS Department offers master of science degrees in computer science, electrical engineering

  4. COMPUTER SCIENCE EECS Department

    E-Print Network [OSTI]

    COMPUTER SCIENCE EECS Department The Electrical Engineering and Computer Science (EECS) Department at WSU offers undergraduate degrees in electrical engineering, computer engineering and computer science. The EECS Department offers master of science degrees in computer science, electrical engineering

  5. Department.: Music Department Course number: 210W

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    Alpay, S. Pamir

    Department.: Music Department Course number: 210W Course title: Music, History, and Ideas Credits: 3 Contact Person: Alain Frogley Catalog Copy: MUSI 210W. Music, History, and Ideas Either semester

  6. Department of Energy | Department of Energy

    Energy Savers [EERE]

    Department of Energy More Documents & Publications Acquisition Letter No. Al 2010-05 Rev 1 - March 20, 2013 Department of Energy Policy Flash 2013-41 Contracts Periods of...

  7. Departement Umweltwissenschaften Department of Environmental Sciences

    E-Print Network [OSTI]

    Fischlin, Andreas

    .......................................................................10 3 The impact of Environmental Sciences graduates on Swiss economy, public administration.............................................................................................................................................. 15 3.1 Four statements on the impact of Environmental Sciences graduates on Swiss economy, publicDepartement Umweltwissenschaften Department of Environmental Sciences Environmental Sciences

  8. Sustainability | Department of Energy

    Office of Environmental Management (EM)

    Sustainability Sustainability The Department of Energy (DOE) supports the understanding and implementation of sustainability programs throughout the complex The Department of...

  9. Nova Biosource Fuels formerly Nova Energy Holding Inc | Open Energy

    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 Inc Jump to:Newberg, Oregon: EnergyNongqishiCleanAlinca Agricola e

  10. department of Civil Engineering

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    U Pat RA department of Civil Engineering Research Activities University of Patras #12;Introduction of our Department and the research activities of the faculty and its graduate students. Civil engineering;Table of Contents Department of Civil Engineering ­ An Introduction 4 Structure of the Department 5

  11. Department Head Resource Portal

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    Salvaggio, Carl

    1 Department Head Resource Portal NEW EMPLOYEE CHECKLIST New Staff Member Name: Department: Start Appearance expectations (e.g., business casual) #12;2 Department Head Resource Portal First Day Prep://myinfo.rit.edu (pay stub, benefits info, emergency contact, etc) Emergency exits #12;3 Department Head Resource Portal

  12. DEPARTMENT OF ECONOMICS AND

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    Kunkle, Tom

    DEPARTMENT OF ECONOMICS AND FINANCE ANNUAL REPORT AY 2013-2014 School of Business 5 Liberty St and change to the Department of Economics and Finance. A revised economics curriculum, a new finance major the department will be divided into two. The Department of Economics will be chaired by Calvin Blackwell

  13. Department of ANIMAL SCIENCE

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    of the Department of Animal science contributes to research-based knowledge on livestock, environment, bioenergy

  14. Nova Era | 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 J APPENDIX ECoop Inc Jump to:Newberg, Oregon: EnergyNongqishiCleanAlinca Agricola eChemicalsEra

  15. Nova Produtiva | Open Energy Information

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    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 Inc Jump to:Newberg, Oregon: EnergyNongqishiCleanAlinca Agricola

  16. Texas Department of State Health Services - WIPP Program | Department...

    Office of Environmental Management (EM)

    Texas Department of State Health Services - WIPP Program Texas Department of State Health Services - WIPP Program Texas Department of State Health Services - WIPP Program More...

  17. Department of Agriculture and Energy Department Announce Up to...

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    Agriculture and Energy Department Announce Up to 8.7 Million through the Interagency Biomass Research and Development Initiative Department of Agriculture and Energy Department...

  18. In: Computer Physics Research Trends ISBN: 978-160021-595-7 Editor: Silvan J. Bianco, pp. 119-150 2007 Nova Science Publishers, Inc.

    E-Print Network [OSTI]

    Yu, Peter K.N.

    TRACK DETECTORS D. Nikezic and K.N. Yu Department of Physics and Materials Science, City University processes, optimization for the measurements, and determination of calibration coefficients in some (222 Rn). The radon gas is originated from the ground and other materials containing its predecessor

  19. THE 2011 ERUPTION OF THE RECURRENT NOVA T PYXIDIS: THE DISCOVERY, THE PRE-ERUPTION RISE, THE PRE-ERUPTION ORBITAL PERIOD, AND THE REASON FOR THE LONG DELAY

    SciTech Connect (OSTI)

    Schaefer, Bradley E.; Landolt, Arlo U. [Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803 (United States); Linnolt, Michael [American Association of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138 (United States); Stubbings, Rod [Tetoora Observatory, Tetoora Road, Victoria (Australia); Pojmanski, Grzegorz [Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa (Poland); Plummer, Alan [Variable Stars South, Linden Observatory, 105 Glossop Road, Linden, NSW (Australia); Kerr, Stephen [American Association of Variable Star Observers, Variable Stars South, Astronomical Association of Queensland, 22 Green Avenue, Glenlee, Queensland (Australia); Nelson, Peter [Ellinbank Observatory, 1105 Hazeldean Road, Ellinbank 3821, Victoria (Australia); Carstens, Rolf [American Association of Variable Star Observers, Variable Stars South, CBA, Geyserland Observatory, 120 Homedale Street, Rotorua 3015 (New Zealand); Streamer, Margaret [Lexy's Palace Observatory, 3 Lupin Place, Murrumbateman, NSW (Australia); Richards, Tom [Variable Stars South, Pretty Hill Observatory, P.O. Box 323, Kangaroo Ground 3097, Victoria (Australia); Myers, Gordon [Center for Backyard Astrophysics, Columbia University, 538 West 120th Street, New York, NY 10027 (United States); Dillon, William G. [American Association of Variable Star Observers, 4703 Birkenhead Circle, Missouri City, TX 77459 (United States)

    2013-08-10

    We report the discovery by M. Linnolt on JD 2,455,665.7931 (UT 2011 April 14.29) of the sixth eruption of the recurrent nova T Pyxidis. This discovery was made just as the initial fast rise was starting, so with fast notification and response by observers worldwide, the entire initial rise was covered (the first for any nova), and with high time resolution in three filters. The speed of the rise peaked at 9 mag day{sup -1}, while the light curve is well fit over only the first two days by a model with a uniformly expanding sphere. We also report the discovery by R. Stubbings of a pre-eruption rise starting 18 days before the eruption, peaking 1.1 mag brighter than its long-time average, and then fading back toward quiescence 4 days before the eruption. This unique and mysterious behavior is only the fourth known (with V1500 Cyg, V533 Her, and T CrB) anticipatory rise closely spaced before a nova eruption. We present 19 timings of photometric minima from 1986 to 2011 February, where the orbital period is fast increasing with P/ P-dot =+313,000 yr. From 2008 to 2011, T Pyx had a small change in this rate of increase, so that the orbital period at the time of eruption was 0.07622950 {+-} 0.00000008 days. This strong and steady increase of the orbital period can only come from mass transfer, for which we calculate a rate of (1.7-3.5) Multiplication-Sign 10{sup -7} M{sub Sun} yr{sup -1}. We report 6116 magnitudes between 1890 and 2011, for an average B = 15.59 {+-} 0.01 from 1967 to 2011, which allows for an eruption in 2011 if the blue flux is nearly proportional to the accretion rate. The ultraviolet-optical-infrared spectral energy distribution is well fit by a power law with f{sub {nu}}{proportional_to}{nu}{sup 1.0}, although the narrow ultraviolet region has a tilt with a fit of f{sub {nu}}{proportional_to}{nu}{sup 1/3}. We prove that most of the T Pyx light is not coming from a disk, or any superposition of blackbodies, but rather is coming from some nonthermal source. We confirm the extinction measure from IUE with E(B - V) = 0.25 {+-} 0.02 mag.

  20. President Obama Named 13 Energy Department Scientists for Outstanding...

    Energy Savers [EERE]

    Department of Agriculture, Department of Commerce, Department of Defense, Department of Education, Department of Energy, Department of Health and Human Services, Department of...

  1. Department of Biomedical Engineering

    E-Print Network [OSTI]

    Stormo, Gary

    Department of Biomedical Engineering Undergraduate Studies Manual 2011­2012 #12;Biomedical Engineering Undergraduate Advising Manual 2011 | 1 Greetings and Department Mission and Objectives 2 Introduction to Biomedical Engineering 3 Biomedical Engineering at Washington University 4 Career Opportunities

  2. Department of Biomedical Engineering

    E-Print Network [OSTI]

    Stormo, Gary

    Department of Biomedical Engineering Undergraduate Studies Manual 2012­2013 #12;Biomedical Engineering Undergraduate Advising Manual 2012 | 1 Greetings and Department Mission and Objectives 2 Introduction to Biomedical Engineering 3 Biomedical Engineering at Washington University 4 Career Opportunities

  3. Department of MINING ENGINEERING

    E-Print Network [OSTI]

    Capecchi, Mario R.

    AS A MINING ENGINEER IMAGINE IMAGINE Department of MINING ENGINEERING THE UNIVERSITY OF UTAH www.mining

  4. DEPARTMENT OF CIVIL ENGINEERING

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    Texas at Arlington, University of

    DEPARTMENT OF CIVIL ENGINEERING 2015 - 2020 Graduate Program Study Planning Guide This document or implied, between and applicant, student, or faculty member, The Department of Civil Engineering a student from whatever penalties he or she may incur. FEBRUARY 2015 #12;DEPARTMENT OF CIVIL ENGINEERING

  5. ACCOUNTING DEPARTMENT UNDERGRADUATE HANDBOOK

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    Alpay, S. Pamir

    1 ACCOUNTING DEPARTMENT UNDERGRADUATE HANDBOOK UNIVERSITY OF CONNECTICUT 2014-2015 #12;2 TABLE OF CONTENTS WELCOME LETTER FROM DEPARTMENT HEAD Page 3 ACCOUNTING DEPARTMENT FACT SHEET Page 4 FACULTY/STAFF Page 6 IMPORTANT RESOURCES Page 7 FREQUENTLY ASKED QUESTIONS Page 10 #12;3 Dear Accounting Majors

  6. Department of Civil, Environmental

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    Department of Civil, Environmental and Geomatics Engineering Annual Report 2000 #12;In the world consequences of this, in October 1999 the former Departments of Civil and Environmental Engineering (D-BAUM) and of Geodesy (D-GEOD) merged to form the new Department of Civil, Environmental and Geomatics Engineering (D

  7. Department of Civil & Environmental

    E-Print Network [OSTI]

    Zhigilei, Leonid V.

    Developing Leaders of Innovation Department of Civil & Environmental Engineering #12;At the U.Va. Department of Civil and Environmental Engineering, our faculty and students serve society's need for sustainable and adaptive infrastructure. #12;Our Students At the U.Va. Department of Civil and Environmental

  8. Department of Energy Facilities | Department of Energy

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    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 DeliciousMathematicsEnergy HeadquartersFuel Cycle |3-938 AUDITResearch | Department ofDepartment

  9. Vehicle Technologies Office News | Department of Energy

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

    November 17, 2015 Energy Department Welcomes Department of Transportation as New Workplace Charging Challenge Partner Today, the Energy Department is welcoming the Department of...

  10. Department of Energy Badges

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

    2000-05-26

    Establishes requirements for Department of Energy (DOE) badges. DOE N 251.40, dated 5/3/01, extends this directive until 12/31/01.

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

    Audience For this ALFAL? Heads of Contracting Activity (HCAs) and Contracting Officers (COs) responsible for administering and managing Department of Energy (DOE) contracts and...

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    ..............................................................................2 Solid Waste Management .........................................................................3 ....................................................................................4 Solid Waste ManagementUnited States Department of Returns on InvestmentsAgriculture Forest Service in Management Sciences

  13. Videos | Department of Energy

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

    Fuel Cell Technology The Energy Department's Fiscal Year 2015 Budget Request Energy 101: Energy Efficient Commercial Buildings Energy 101: Energy Efficient Commercial Buildings...

  14. Blog | Department of Energy

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

    reflective coatings on windows, exterior walls, and roofs to provide comfort during the cooling season. | Photo courtesy of Jason Flakes, U.S. Department of Energy Using Passive...

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

    in the production of clean energy technologies like electric vehicles, LED bulbs and solar panels. The Department is also working with manufacturers to increase their energy...

  16. United States Department of

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    United States Department of Agriculture Forest Service Pacific Southwest Research Station General assigned to the Station's research unit studying the regeneration of California forests

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    United States Department of Agriculture MIX: A Computer Program to Evaluate Forest Service, a research entomologist, is in charge of the unit developing improved technology for integrated management

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    United States Department of Agriculture Forest Service Pacific Southwest Research Station General Programs: A Review of Cognitive and Behavioral Studies Introduction Recent wildfires in the Western United

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    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range to the Chaparral Prescribed Fire Research Unit, headquartered at Riverside, California. Publisher: Pacific

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    United States Department of Agriculture Forest Service Pacific Southwest Research Station General is a Research Ecologist at the Station's Timber Management/Wildlife Habitat Interactions Unit, Redwood Sciences

  1. United States Department of

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    Kurapov, Alexander

    A United States Department of Agriculture Forest Service Pacific Northwest Research Station General, land management, carbon sequestration, carbon markets, United States. #12;ii Executive Summary

  2. United States Department of

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    United States Department of Agriculture Forest Service Intermountain Research Station General acrossthe United States provide estimates of the amount of erosion reductionon forest roadsfrom

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    94701 United States Department of Agriculture Forest Service Pacific Southwest Forest and Range of California, Berkeley, and a cooperator with the Research Unit. #12;Acknowledgments We especially acknowledge

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    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range to the Station's chaparral and related ecosystems research unit, with headquarters at Riverside, California. He

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    United States Department of California Oaks: A Bibliography Agriculture Forest Service Pacific forester in the Station's Forest Regeneration Research Unit, at Redding, California. He holds bachelor

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    Wang, Changlu

    United States Department of Agriculture Rural Business- Cooperative Service Research Report 157, concentration, globalization, agency theory Cooperatives in a Changing Global Food System United States

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    United States Department of Agriculture Forest Service Pacific Southwest Research Station General is a supervisory research entomologist in the Station's Regeneration Insect Research Unit in Berkeley. W. WAYNE

  8. Department of Biomedical Engineering

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    Zhigilei, Leonid V.

    Department of Developing Leaders of Innovation Biomedical Engineering #12;At U.Va., biomedical and techniques of biomedical engineering -- molecular biology, cellular microscopy, cell and tissue mechanics

  9. Department of Energy (DOE) Acquisition Guide | Department of...

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  10. Oregon Department of Land Conservation and Department - Forest...

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    MAINTENANCE (Purchasing Department) vs. CONSTRUCTION (Design & Construction Services Department NO NO Maintenance or Construction Decision Tree Maintenance : Maintenance is the upkeep of property , machinery

  12. Stuttgart University The Department of

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    Reyle, Uwe

    Stuttgart University 2010 The Department of Geodesy and Geoinformatics #12;editing and layout highlights of the Department of Geodesy & Geoinformatics of the University of Stuttgart. The Department report documents our research contributions in many diverse fields of Geodesy & Geoinformatics: from

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    Toronto, University of

    datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING UNIVERSITY OF TORONTO 2006 TRANSPORTATION Group Department of Civil Engineering University of Toronto July 2009 #12;i ACKNOWLEDGMENTS The 2006 Management Group (DMG) at the Department of Civil Engineering, University of Toronto. The Steering Committee

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    DBAUG Department of Civil, Environmental and Geomatic Engineering DEVELOPMENT OF A NEW LASER #12;DBAUG Department of Civil, Environmental and Geomatic Engineering Outline Introduction;DBAUG Department of Civil, Environmental and Geomatic Engineering Introduction Optical indoor

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    Department of Mechanical and Automation Engineering #12;4 2 3 1 Contents Messages in the souvenir publication of the Department of Mechanical and Automation Engineering of The Chinese University of Mechanical and Automation Engineering have also played a significant part in equipping businesses

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    Huang, Wei

    Developing Leaders of Innovation Department of Science, Technology, & Society #12;Understanding the relationship between technology and society is crucial to becoming a successful leader in any field. #12;Our Students The University of Virginia Department of Science, Technology, and Society offers a comprehensive

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    Zhigilei, Leonid V.

    Developing Leaders of Innovation Department of Chemical Engineering #12;At the University of Virginia, we educate students in traditional and nontraditional areas of chemical engineering, giving them.Va. Department of Chemical Engineering benefit from a modern academic curriculum and state

  18. United States Department of

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    Holberton, Rebecca L.

    United States Department of Agriculture Forest Service Northeastern Research Station General Technical Report NE-318 Atlas of Climate Change Effects in 150 Bird Species of the Eastern United States Service 359 Main Road Delaware, OH 43015 USA #12;United States Department of Agriculture Forest Service

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    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 tCorporation |Inc.: Federal Register Notice,L.L.C.

  20. Financial Opportunities | Department of Energy

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    6, 2015 Energy Department Awards 7.4 Million to Develop Advanced Components for Wave and Tidal Energy Systems The Energy Department today announced four entities selected to...

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    Department of Statistics STATISTICS COLLOQUIUM GOURAB MUKHERJEE Department of Statistics Stanford directions in statistical probability forecasting. Building on these parallels we present a frequentist

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    E-Print Network [OSTI]

    Department of Statistics STATISTICS COLLOQUIUM INGRAM OLKIN Department of Statistics Stanford probability, statistics, combinatorics and graphs, numerical analysis and matrix theory. Special emphasis

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    Department of Statistics STATISTICS COLLOQUIUM ZONGMING MA Department of Statistics University (CCA) is a widely used multivariate statistical technique for exploring the relation between two sets

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    Dobrotka, A

    2015-01-01

    An optical light curve of SU UMa type dwarf nova V1504 Cyg taken by Kepler was analysed in order to study fast optical variability (flickering). We calculated power density spectra and rms-flux relations for two different stages of activity, i.e. quiescence and regular outbursts. A multicomponent power density spectrum with two break frequencies was found during both activity stages. The rms-flux relation is obvious only in the quiescent data. However, while the collection of all outburst data do not show this variability, every individual outburst does show it in the majority of cases keeping the rms value approximately in the same interval. Furthermore, the same analysis was performed for light curve subsamples taken from the beginning, middle and the end of the supercycle both for quiescence and regular outbursts. Every light curve subsample shows the same multicomponent power density spectrum. The stability of the break frequencies over the supercycle can be confirmed for all frequencies except for the hi...

  8. Climate Workshops for Department Chairs Introduction

    E-Print Network [OSTI]

    Sheridan, Jennifer

    #12;Climate Workshops for Department Chairs Introduction Why focus on Department Chairs? Goals participating departments Evidence from Campus-wide Climate Surveys #12;Why focus on Department Chairs? Individuals experience climate in their immediate workplace ­ the department Chairs can significantly

  9. Department 2 Taxation, Accounting and Finance

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    Hellebrand, Sybille

    Department 2 Taxation, Accounting and Finance #12;Department 2: Taxation, Accounting and Finance 2, Investition #12;Department 2: Taxation, Accounting and Finance 3 Übersicht Lehrstühle des Department 2 Prof #12;Department 2: Taxation, Accounting and Finance 4 Finanzwirtschaft und Bankbetriebslehre

  10. Psychology Department Bylaws Page 1 DEPARTMENT OF PSYCHOLOGY

    E-Print Network [OSTI]

    Walker, Lawrence R.

    Psychology Department Bylaws Page 1 DEPARTMENT OF PSYCHOLOGY BYLAWS Updated through 8 1.1 The Departmental Bylaws, day-to-day operations and administration of the Psychology Department Responsibilities of the Faculty 2.1 The faculty of the Psychology Department, acting as a group, has

  11. Services | Department of Energy

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  12. Vacancies | Department of Energy

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  13. Videos | Department of Energy

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    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 JacksonDepartment| Department of Energy OfficeResourcesmap|DepartmentThe Hanford

  14. Videos | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department of Energy OfficeResourcesmap|DepartmentThe HanfordNew

  15. Videos | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department of Energy OfficeResourcesmap|DepartmentThe

  16. Videos | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department of Energy OfficeResourcesmap|DepartmentTheVideo Title

  17. 1 | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department of EnergyDataWindofEDT | Department0980_001.pdf/ The1

  18. Fossil | 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 GasAdjustmentsShirley Ann JacksonDepartment of Energy Facilities ByDepartmentOffice of| DepartmentSince

  19. DEPARTMENT OF CIVIL, ENVIRONMENTAL AND

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    DEPARTMENT OF CIVIL, ENVIRONMENTAL AND GEOMATICS ENGINEERING ANNUAL REPORT 2004 #12;3 The Department of Civil, Environmental and Geomatic Engineering of ETH Zurich exists since October 1999, as a result of the fusion of the Department of Civil and Environmental Engineering with the Department

  20. Department of Economics Financial Aid

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    Huang, Haiying

    Department of Economics Financial Aid: Availability and Requirements in the Department of Economics The Department of Economics has several sources of financial aid for domestic and international students Assistantships in the Department of Economics The predominant form of financial aid is the graduate research

  1. Department of Energy

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

    Energy.gov Solar Decathlon 2015 Solar Decathlon 2015 The competition is heating up at U.S. Department of Energy Solar Decathlon 2015 Go to energy.govsolardecathlon for full...

  2. Blog | Department of Energy

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

    salute to the Department of Defense for their heroic efforts when it comes to saving electrons. November 10, 2015 An insulated door was an easy upgrade from the steel cellar door...

  3. DEPARTMENTS Architecture & Civil Engineering

    E-Print Network [OSTI]

    Burton, Geoffrey R.

    DEPARTMENTS Architecture & Civil Engineering Biology & Biochemistry Chemical Engineering Chemistry Computer Science Economics Education Electronic & Electrical Engineering Politics, Languages and International Studies School of Management Mathematical Sciences Mechanical Engineering (Sports Engineering

  4. Department of Systems & Information

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    Zhigilei, Leonid V.

    , communication systems, control systems, economic systems, energy and environmental systems, human factors systems, safety-critical systems, wireless communications, game theory and artificial intelligenceDeveloping Leaders of Innovation Department of Systems & Information Engineering #12;In the U

  5. United States Department of

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    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range symposium dealing with this subject in the western United States, the papers presented address current ........................................................................................................................................ 1 Annosus Root Disease in Europe and the Southeastern United States: Occurrence, Research

  6. United States Department of

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    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range, objectives, and targets and specific work plans for the field units--the National Forests and their Ranger

  7. United States Department of

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    United States Department of Agriculture Forest Service Northeastern Forest Experiment Station research unit in New Hampshirein 1957, where he studied problemsof regenerationandthinning research unit at Warren, Pennsylvania, where he headed a program of research on problems related

  8. United States Department of

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    United States Department of Agriculture Forest Service Pacific Northwest Research Station Research, and export from 1997 to 2010, for main world regions and the United States. Detailed tables by country

  9. United States Department of

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    United States Department of Agriculture Forest Service Peelflc Southwest Forest and Range that are expressed in tems familim to the user. Theboard footand cubic footare mdiriond units of measure, altlnough

  10. United States Department of

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    United States Department of Agriculture Forest Service Northeastern Research Station Research Paper-Central United States (Monserud and Ek 1977; Monserud 1987). This model was used within the framework of FOREST

  11. United States Department of

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    #12;United States Department of Agriculture Forest Service Pacific Southwest Research Station for the Station's Wildland Recreation and the Urban Culture Research Work Unit, located at the Forest Fire

  12. United States Department of

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    United States Department of Agriculture Usual Planting and Harvesting Dates for U.S. Field Crops million acres of barley were harvested in the United States (U.S.) during 1996. After reaching a peak

  13. United States Department of

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    United States Department of Agriculture Forest Service Pacific Northwest Research Station Research, import, and export from 1997 to 2010, for main world regions and the United States. Detailed tables

  14. Department of Materials Science &

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    Zhigilei, Leonid V.

    Developing Leaders of Innovation Department of Materials Science & Engineering #12;At the University of Virginia, students in materials science, engineering physics and engineering science choose to tackle compelling issues in materials science and engineering or engineering science

  15. Department of Mechanical & Aerospace

    E-Print Network [OSTI]

    Zhigilei, Leonid V.

    in mechanics, electrical theory, kinematics, thermodynamics, fluid mechanics, heat transfer and materials dynamics, fluid dynamics, propulsion and structures. While each program features a solid technicalDeveloping Leaders of Innovation Department of Mechanical & Aerospace Engineering #12;Emphasizing

  16. United States Department

    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 |RecordsDepartment ofEnergyDepartmentDepartmentofALA-1-NWashington,

  17. Cathodes | 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:FinancingPetroleum Based Fuels|Programs | DepartmentDepartment of EnergyWyomingNationalCathodes

  18. Autotune | 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:FinancingPetroleum Based Fuels Research atDepartmentAuditsDepartment of(TEG)ofAutotune

  19. Dehumidifiers | 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:FinancingPetroleum Based| Department8, 20153Daniel BoffDepartment ofCondition |

  20. 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:FinancingPetroleum Based| Department8, 20153Danielthrough the InteragencyDepartment's Freedom of

  1. 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:FinancingPetroleum Based| Department8, 20153Danielthrough the InteragencyDepartment's Freedom

  2. 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:FinancingPetroleum Based| Department8, 20153Danielthrough the InteragencyDepartment's Freedom09

  3. Department of Energy (DOE)

    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:FinancingPetroleum Based| Department8, 20153Danielthrough the InteragencyDepartment's Freedom09

  4. Department of Energy - Blog

    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:FinancingPetroleum Based| Department8, 20153Danielthrough the InteragencyDepartment's Freedom097 en

  5. Dispatchability | 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:FinancingPetroleum Based| Department8,Department of Energy2EM's CleanupPower »

  6. Document | Department of Energy

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

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  7. Durability | Department of Energy

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

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  8. Publications | 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 DeliciousMathematicsEnergyInterested PartiesBuildingBudget || Department ofDepartmentEnergy Policy Act

  9. Newsletters | Department of Energy

    Energy Savers [EERE]

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  10. Insulation | Department of Energy

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

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  11. Insurance | Department of Energy

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  12. Dashboards | Department of Energy

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  13. Publications | Department of Energy

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

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  14. Publications | Department of Energy

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

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  15. Education | Department of Energy

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

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  16. Inspector | Department of Energy

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

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  17. Insulation | Department of Energy

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

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  18. Department of Energy | 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:FinancingPetroleum Based| Department8, 20153Danielthrough theK APolicyon December 8, 2010AL

  19. Department of Energy | 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:FinancingPetroleum Based| Department8, 20153Danielthrough theK APolicyon December 8, 2010ALMore

  20. Department of Energy | 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:FinancingPetroleum Based| Department8, 20153Danielthrough theK APolicyon December 8,

  1. Procedures for Departing Employees | Department of Energy

    Energy Savers [EERE]

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  2. NNSA Administrator to Depart | Department of Energy

    Energy Savers [EERE]

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  3. Procedures for Departing Employees | Department of Energy

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

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  4. Department of Energy No | Department of Energy

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

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  5. Department of Energy Accomplishments | 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 pStateDOEAnalysis,DepartmentAboveProgram to Assist7 enSustainabilityDOE

  6. Department of Energy | 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:FinancingPetroleum Based| Department8, 20153Danielthrough theK APolicyon December 8, 2010AL 2008-02

  7. Department of Energy Facilities | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice ofof Energy Brad BuggerOIGM.DenverWorker

  8. DEPARTMENT OF CHEMICAL ENGINEERING DEPARTMENT OF MECHANICAL AND INDUSTRIAL ENGINEERING

    E-Print Network [OSTI]

    Mountziaris, T. J.

    DEPARTMENT OF CHEMICAL ENGINEERING DEPARTMENT OF MECHANICAL AND INDUSTRIAL ENGINEERING University review of kinetic processes in engineering materials that control the materials' structural and chemical in engineering materials that control the materials' structural and chemical characteristics in relation

  9. DEPARTMENT OF CHEMICAL ENGINEERING DEPARTMENT OF MECHANICAL AND INDUSTRIAL ENGINEERING

    E-Print Network [OSTI]

    Mountziaris, T. J.

    DEPARTMENT OF CHEMICAL ENGINEERING DEPARTMENT OF MECHANICAL AND INDUSTRIAL ENGINEERING University aims at a comprehensive introduction to the mechanical behavior of solid engineering materials utilized. Understanding of the mechanical behavior of solid engineering materials used in current materials engineering

  10. Department of Energy National Science Bowl | Department of Energy

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

    Department of Energy National Science Bowl Department of Energy National Science Bowl May 5, 2008 - 11:30am Addthis Remarks as Prepared for Delivery by Secretary Bodman Thank you,...

  11. DEPARTMENT EMERGENCY ACTION PLAN Department Name: IAB Greenhouse

    E-Print Network [OSTI]

    DEPARTMENT EMERGENCY ACTION PLAN For Department Name: IAB Greenhouse Date DEAP Adopted: January 24 Greenhouse Building address: 911 Yukon Drive Building coordinator: Mark Wright Building coordinator telephone assembly locations Inside assembly location: Butrovich lobby Outside assembly location: IAB Greenhouse

  12. Steel | 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 RankADVANCED MANUFACTURINGEnergyPlan | Department of Energy 1 DOE| Department ofSteam SystemSteamSteel

  13. Conferences | 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 aDepartment ofCommercialEnergyDepartment ofHeating

  14. Transmission | 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 GasAdjustmentsShirleyEnergyThe U.S.Laclede GasEfficiency| DepartmentSecurity | Department of

  15. Mission | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice| DepartmentGJPPGPracticesDraft.doc Moreof% of Careers &

  16. Mission | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice| DepartmentGJPPGPracticesDraft.doc Moreof% of Careers

  17. Mission | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice| DepartmentGJPPGPracticesDraft.doc Moreof% of CareersMission

  18. News | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice|in the subsurface isProject | Department of Energy

  19. News | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice|in the subsurface isProject | Department of EnergyStay

  20. News | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice|in the subsurface isProject | Department ofNewsDecember 16,

  1. Outreach | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice|in theLegislative Documents USU.S. DepartmentOrganizationDOE)

  2. STILE | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice|inWestMay 13, 2015reports issuedExperience | Department|STILE

  3. Wind | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department of EnergyDataWind The United States is home to one of

  4. AIRMaster+ | 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 GasAdjustmentsShirley Ann JacksonDepartment| Department ofApplianceU.S.Departmentthe(RevisionU.S.appearing

  5. Blog | 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 GasAdjustmentsShirley Ann JacksonDepartment of Energy Facilities By E-mail: YouAbsorptionDepartment ofBetterof

  6. Homes | 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 GasAdjustmentsShirley Ann JacksonDepartment of Energy Facilities ByDepartmentOfficeTheAllison Lanteroleads a

  7. Enforcement | 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 GasAdjustmentsShirley Ann JacksonDepartment ofOffice ofofWind ProjectsEfficiencyPreparedKY The City4,| Department

  8. U.S. DEPARTMENT OF Message from the Department of

    E-Print Network [OSTI]

    Pennycook, Steve

    #12;ENERGY U.S. DEPARTMENT OF Message from the Department of Energy and the National Nuclear energy. The information presented in this summary shows that Oak Ridge is a safe community for its Security Administration Each year the Department of Energy conducts environmental monitoring at each

  9. Department of Geography By-Laws 2007 Department of Geography

    E-Print Network [OSTI]

    McQuade, D. Tyler

    Department of Geography By-Laws 2007 1 By-Laws Department of Geography Florida State University 2017 unless reviewed and approved by a majority of faculty The mission of the Department of Geography in geography and related disciplines; and to be available as a public service to the local community. These by

  10. Mechanical Engineering Department 03 November 2014

    E-Print Network [OSTI]

    Furlong, Cosme

    Mechanical Engineering Department Lecture 02 03 November 2014 WORCESTER POLYTECHNIC INSTITUTE MECHANICAL ENGINEERING DEPARTMENT Optical Metrology and NDT ME-593L, B'2014 #12;Mechanical Engineering Department Light Sources Electromagnetic spectrum #12;Mechanical Engineering Department Light Sources

  11. Whitacre College of Engineering Industrial Engineering Department

    E-Print Network [OSTI]

    Gelfond, Michael

    Whitacre College of Engineering Industrial Engineering Department Department Chair and Professor of Industrial Engineering. The Industrial Engineering Department at Texas Tech University has a distinguished industrial engineering education and provide appropriate service to the department, university

  12. GRADUATE STUDENT Department of Physics

    E-Print Network [OSTI]

    Zallen, Richard

    General Policies and Procedures The Physics department offers M.S. and Ph.D. degrees in physicsGRADUATE STUDENT HANDBOOK Department of Physics Virginia Polytechnic Institute and State University November 2014 #12;2 _________________________________________________________________ Virginia Tech Physics

  13. Ankit Kalani Department of Mechanical

    E-Print Network [OSTI]

    Kandlikar, Satish

    Ankit Kalani Department of Mechanical Engineering & Microsystems Engineering, Rochester Institute of Technology, Rochester, NY 14623 e-mail: axk2161@rit.edu Satish G. Kandlikar1 Department of Mechanical

  14. Civil Engineering Department ADVISING CONTRACT

    E-Print Network [OSTI]

    Maxwell, Bruce D.

    Civil Engineering Department ADVISING CONTRACT When you seek pre-registration or registration and will be reported to the Assistant Dean. A student may petition the Civil Engineering Department Head for a waiver

  15. Psychology Department Mandatory Advising Requirement

    E-Print Network [OSTI]

    10/2011 Psychology Department Mandatory Advising Requirement Instructions 1) Student completes Part advisor's signature. 4) Once the form is signed, submit form to Psychology Department, EP 301 to clear

  16. Department of Mathematics: Old Exams

    E-Print Network [OSTI]

    Department of Mathematics. Search field. About Us · Faculty · Emeritus Faculty · Visiting Scholars · Lecturers · Graduate Students · Other Teaching Assistants ...

  17. Tax Credits, Rebates & Savings | Department of Energy

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

    Tax Credits, Rebates & Savings Reading Municipal Light Department- Business Lighting Rebate Program Reading Municipal Light Department (RMLD) offers incentives for...

  18. Tax Credits, Rebates & Savings | Department of Energy

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

    Rebates & Savings Marblehead Municipal Light Department- Residential Energy Efficiency Rebate Program Marblehead Light Department encourages conservation within the residential...

  19. Energy Department's Loan Portfolio Continues Strong Performance...

    Office of Environmental Management (EM)

    Department's Loan Portfolio Continues Strong Performance While Deploying Innovation Energy Department's Loan Portfolio Continues Strong Performance While Deploying Innovation...

  20. Department of Industrial and Systems Engineering Discussion ...

    E-Print Network [OSTI]

    2009-02-23

    Feb 23, 2009 ... Japan. 1Department of Industrial and Systems Engineering, Chuo University. 2Department of Administration Engineering, Keio University ...

  1. Actuarial Science Program - Department of Mathematics, Purdue ...

    E-Print Network [OSTI]

    $author.value

    The Purdue Actuarial Science Program is an interdisciplinary program offered jointly by the Department of Mathematics and Department of Statistics.

  2. Stuttgart University The Department of

    E-Print Network [OSTI]

    Reyle, Uwe

    Stuttgart University 2009 The Department of Geodesy and Geoinformatics #12;editing and layout highlights of the Department of Geodesy & Geoinformatics of Universit¨at Stuttgart. The Depart- ment consists contributions in many diverse fields of Geodesy & Geoinformatics: from satellite and physical geodesy through

  3. Stuttgart University The Department of

    E-Print Network [OSTI]

    Reyle, Uwe

    Stuttgart University 2006 The Department of Geodesy and Geoinformatics #12;editing and layout highlights of the Department of Geodesy and Geoinformatics of Universit¨at Stuttgart. The Depart- ment documents our research contributions in many diverse fields of Geodesy and Geoinformatics: from satellite

  4. Stuttgart University The Department of

    E-Print Network [OSTI]

    Reyle, Uwe

    Stuttgart University 2007 The Department of Geodesy and Geoinformatics #12;editing and layout highlights of the Department of Geodesy and Geoinformatics of Universit¨at Stuttgart. The Depart- ment diverse fields of Geodesy and Geoinformatics: from satellite and physical geodesy through navigation

  5. Stuttgart University The Department of

    E-Print Network [OSTI]

    Reyle, Uwe

    Stuttgart University 2008 The Department of Geodesy and Geoinformatics #12;editing and layout highlights of the Department of Geodesy & Geoinformatics of Universit¨at Stuttgart. The Depart- ment consists documents our research contributions in many diverse fields of Geodesy & Geoinformatics: from satellite

  6. datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING

    E-Print Network [OSTI]

    Toronto, University of

    datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING UNIVERSITY OF TORONTO 2006 TRANSPORTATION Committee by the Data Management Group Department of Civil Engineering University of Toronto June 2009 #12;i Group Department of Civil Engineering University of Toronto 35 St. George Street Toronto, Ontario M5S 1A

  7. datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING

    E-Print Network [OSTI]

    Toronto, University of

    datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING UNIVERSITY OF TORONTO 2006 TRANSPORTATION Committee by the Data Management Group Department of Civil Engineering University of Toronto July 2009 #12;i Group Department of Civil Engineering University of Toronto 35 St. George Street Toronto, Ontario M5S 1A

  8. datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING

    E-Print Network [OSTI]

    Toronto, University of

    datamanagementgroup DEPARTMENT OF CIVIL ENGINEERING UNIVERSITY OF TORONTO 2006, 2001, 1996 and 1986 for the Transportation Information Steering Committee by the Data Management Group Department of Civil Engineering Management Group (DMG) at the Department of Civil Engineering, University of Toronto. The Steering Committee

  9. United States Department of Agriculture

    E-Print Network [OSTI]

    Gray, Matthew

    United States Department of Agriculture Keys to Soil Taxonomy Ninth Edition, 2003 #12;#12;Keys to Soil Taxonomy By Soil Survey Staff United States Department of Agriculture Natural Resources Conservation Service Ninth Edition, 2003 #12;The United States Department of Agriculture (USDA) prohibits

  10. Department of Computer 2014 2015

    E-Print Network [OSTI]

    Delene, David J.

    Department of Computer Science 2014 ­ 2015 Scholarship Application #12;Department of Computer Science Academic Year 2014-2015 Scholarship Program The Department of Computer Science makes scholarships are committed to rewarding students majoring in Computer Science who have demonstrated a high degree

  11. Department of Polymer Science

    E-Print Network [OSTI]

    Dhinojwala, Ali

    Department of Polymer Science The University of Akron, OH 330-972-6246 ali4@uakron.edu www2.uakron to develop synthetic adhesives and coatings. He has patents in carbon nanotube- based adhesives and coatings of molecules at the interface. The Dhinojwala laboratory has developed SFG technique to study polymer

  12. United States Department of

    E-Print Network [OSTI]

    North, Malcolm

    for Sierran Mixed- Conifer Forests Malcolm North, Peter Stine, Kevin O'Hara, William Zielinski, and Scott Park Drive, Davis, CA 95618, mpnorth@ucdavis.edu, pstine@fs.fed.us. Kevin O'Hara is a professor@nature.berkeley.edu, stephens@ nature.berkeley.edu. William Zielinski is a research ecologist, U.S. Department of Agriculture

  13. Honoring Energy Department Vets

    SciTech Connect (OSTI)

    Chu, Steven; Majors, Alvan; Underwood, David

    2012-01-01

    Veterans from the Army, Air Force, Navy, Marine Corps and the National Guard who work at the Department of Energy met Wednesday with Secretary Steven Chu, who hosted more than a dozen former service members to thank them for their continued service to America.

  14. Department of Computer Science

    E-Print Network [OSTI]

    North, Siobhán

    Department of Computer Science Retrieving Software Component using Clone Detection and Program appropriate software components in a library or software component retrieval are an important task in software features using clone detection technique, (iii) searching components in the library based on the clone

  15. ETSU Department of Sustainability

    E-Print Network [OSTI]

    Karsai, Istvan

    ETSU Department of Sustainability Kathleen Moore- Director of Sustainability MOORE@mail.etsu.edu 423-439-7766 Jared Jones- Coordinator, Eco Nuts jonesjm@goldmail.etsu.edu 423-433-3493 Please email How To Apply gogreen@etsu.edu requesting an application. A completed application including a resume

  16. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range unit investigating measurement and analysis techniques for management planning, with headquarters in Berkeley, Calif. ELLIOT L. AMIDON is now assigned to the Station's unit at Arcata, Calif., that is studying

  17. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Northeastern Research Station General Estimates for Forest Types of the United States James E. Smith Linda S. Heath Kenneth E. Skog Richard A forest types within 10 regions of the United States. Separate tables were developed for afforestation

  18. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service General Technical #12;- TH ,a geneticist, is assigned to the Station's research unit dyin etics of western forest trees, with headquarters in Berkeley, Berkeley. PAUL D. cal technician with the genetics research unit, isa forestry gra California, Berkeley

  19. United States Department of

    E-Print Network [OSTI]

    Clements, Craig

    United States Department of Agriculture Forest Service Intermountain Research Station Ogden, UT. He was project leader of the fire fundamentals research work unit from 1966 until 1979 and is currently project leader of the fire behavior research work unit at the fire sciences laboratory. RALPH A

  20. United States Department of

    E-Print Network [OSTI]

    Liebhold, Andrew

    United States Department of Agriculture Forest Service Northeastern Research Station Research Paper of the Eastern United States have been devastated by invasive pests. We used existing data to predict-quarter in total host density. Gypsy moth occupies only 23 percent of its potential range in the Eastern United

  1. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range Thomas J. Mills Frederick W. Bratten #12;The Authors: are with the Station's research unit studying fire J. MILLS, a forest economist, is in charge of the unit. He earned degrees at Michigan State

  2. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Pacific Southwest Forest and Range ecosystemsresearch unit located in Riverside. California. PAUL H. DUNN was project leader at that time and is now project leader of the atmospheric deposition research unit in Riverside. Calif. SUSAN C. BARRO

  3. United States Department of

    E-Print Network [OSTI]

    United States Department of Proceedings of the Agriculture Pacific Southwest Symposium on Social of Agriculture; 96 p. The growing demand for recreation at the wildland-urban interface throughout the United and the Urban Culture Research Unit headquartered at the Forest Fire Laboratory, 4955 Canyon Crest Dr

  4. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Pacific Southwest Research Station http. Arbaugh is a statistician with the Station's Atmospheric Deposition Effects Research Unit at Riverside and associate professor with the National Park Service Cooperative Park Studies Unit, College of Forest

  5. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Northeastern Research Station Research Paper NE-722 James E. Smith Linda S. Heath A Model of Forest Floor Carbon Mass for United States Forest contiguous United States. Manuscript received for publication 22 April 2002 #12;A Model of Forest Floor

  6. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Southern Research Station General Technical United States. In: Rauscher, H. Michael, and Kurt Johnsen, eds. Southern forest science: past, present Trends in the Southern United States Robert A. Mickler, James E. Smith, and Linda S. Heath1 Abstract

  7. United States Department of

    E-Print Network [OSTI]

    United States Department of Agriculture Forest Service Northeastern Research Station General reported in USDA Forest Service surveys for forests of the conterminous United States. Developed for use estimates are provided for regional tree-mass totals using summary forest statistics for the United States

  8. Department of Environmental

    E-Print Network [OSTI]

    Zeng, Ning

    Department of Environmental Safety DIVISION OF ADMINISTRATIVE AFFAIRS LOCKOUT TAGOUT PLAN (CONTROL, MD 20742-3133 (301) 405-3960 FAX (301) 314-9294 #12;#12;Lockout Tagout Program i Table of Contents Implementing Lockout/Tagout 7 I. Preparation for Shutdown 8 II. Shutdown of Machine 8 III. Return Equipment

  9. Department Seal and Flag

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

    1992-05-18

    This directive sets forth the policy governing the use of the official seal and distinguishing flag of the Department of Energy (DOE) as described in Title 10, Code of Federal Regulations (CFR), Part 1002. Cancels DOE O 10002.A dated 1-8-90.

  10. Honoring Energy Department Vets

    ScienceCinema (OSTI)

    Chu, Steven; Majors, Alvan; Underwood, David;

    2013-05-29

    Veterans from the Army, Air Force, Navy, Marine Corps and the National Guard who work at the Department of Energy met Wednesday with Secretary Steven Chu, who hosted more than a dozen former service members to thank them for their continued service to America.

  11. Department of Defense INSTRUCTION

    E-Print Network [OSTI]

    US Army Corps of Engineers

    of the Inspector General of the Department of Defense, the Defense Agencies, the DoD Field Activities, and all of the DoD VE Program. b. Implements the reporting requirements of Reference (c). c. Establishes referred to in paragraph 2f of Enclosure 3 of this instruction has been assigned report control symbol DD

  12. Civil & Environmental Engineering Department

    E-Print Network [OSTI]

    Bertini, Robert L.

    Civil & Environmental Engineering Department 2012 Porfolio www.pdx.edu/cee This portfolio 40 45 50 55 60 65 70 75 80 85 90 Passingrate% Environmental FE Exam Afternoon Pass Rate ComparisonPassing,% Environmental Engineering FE Exam Comparison of Pass Rates PSU Results National Results #12;Current Faculty

  13. DEPARTMENT OF STRATEGIC PLAN

    E-Print Network [OSTI]

    Virginia Tech

    to effectively manage forest and allied natural resources. This revised strategic plan reiterates our commitment is to educate foresters and natural resource managers, and to discover and disseminate the knowledge needed has matured and grown and is now one of four departments in the College of Natural Resources

  14. Department of Bioengineering Engineering

    E-Print Network [OSTI]

    Fang-Yen, Christopher

    Department of Bioengineering Engineering Penn INVENT | CREATE | DISCOVER #12;"My research allows me to directly apply my bioengineering education, to think critically and develop and test new methods to answer Ivy League university and a top international research and medical community. In bioengineering, you

  15. Department COAP Chairs in PSOM Departments Department COAP Chair Phone Email

    E-Print Network [OSTI]

    Sharp, Kim

    Department COAP Chairs in PSOM Departments Department COAP Chair Phone Email Anesthesia@exchange.upenn.edu Cell & Developmental Biology Stephen DiNardo, PhD 898-1367 sdinardo@mail.med.upenn.edu Dermatology John-8014 cjd@mail.med.upenn.edu Psychiatry Karl Rickels, MD 746-6417 krickels@mail.med.upenn.edu Radiation

  16. Computer Physics Communications 30 (1983) 255--257 255 North-Holland Publishing Company

    E-Print Network [OSTI]

    Creutz, Michael

    1983-01-01

    * Michael CREUTZ Department of Physics, Brookhaven National Laboratory, Upton, NY 11973, USA and K Scotia, Canada B3H 4H8 Received 30 June 1983; in revised form 11 July 1983 ADAPTATION SUMMARY Title calculations. We wish to apply this technique to Adaption number: 0001 SU(3) gauge theory. Programs obtainable

  17. Recent developments: Industry briefs

    SciTech Connect (OSTI)

    1990-04-01

    Recent nuclear industry briefs are presented. These briefs include: Soviet Union to build Iran nuclear plant; Dension announces cuts in Elliot Lake production; Soviet environmental study delays Rostov startup; Cogema closes two mines; Namibian sanctions lifted by USA and Canada; US Energy and Kennecott restructors joint venture; Australians reelect Hawke; China to buy Soviet nuclear plant; Olympic Dam`s first sale of concentrates to USA; Uranevz buys one-third of Cogema`s Rabbit Lake operations; East and West Germany forming joint nuclear law; and Nova Scotia extends uranium exploration plan.

  18. Horticultural Survey of Gulf Coast. 

    E-Print Network [OSTI]

    Green, Edward C.

    1907-01-01

    e.-lst, cabbage; 2nd, onions; 3rd, Irish potatoes; 4th, CU- cumbers. Sarlta Maria.-lst, onions; 2nd, cucumbers; 3rd, beans; 4th, cabbage. While there is .some difference of opinion among inaiuiduals as to the relative value and profit in certain..., and to Halifax, Nova Scotia, as well as to other markets less distant. SANTA MARIA. For rapid development from 'brush and cactus to in- tensified profitable gardening Kingsville made a two-year record which probably had never been equalled up to that time...

  19. Roadmaps | 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 Tool FitsProject DevelopsforReportingResourcesDepartment ofEnvironments

  20. Partnerships | 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 DeliciousMathematics AndBeryllium Disease | DepartmentOLED StakeholderINL E-IDREnergy Partnerships Help