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1

First results from the MACRO (Monopole, Astophysics, Cosmic Ray Observatory) detector at the Gran Sasso Laboratory  

Science Conference Proceedings (OSTI)

The MACRO (Monopole, Astrophysics, Cosmic Ray Observatory) detector which is being installed at the underground Gran Sasso Laboratory (LNGS) is described in detail. The performance of the detector's first supermodule ({approximately}800 m{sup 2}sr), which had its initial data run from February 27 to May 30, 1989, is reported. About 245,000 muon triggers were recorded during this first run. Preliminary results are presented on: the measured vertical muon flux; the detection features of MACRO as a high energy muon and muon neutrino telescope; the measured lateral spread and multiplicity distributions of muon bundles; a search for GUT magnetic monopoles; a search for electron anti-neutrinos from stellar collapses. In addition, there are results obtained in conjunction with the EAS-TOP detector located on top of the Gran Sasso mountain. 24 refs., 22 figs.

Calicchio, M.; De Cataldo, G.; De Marzo, C.; Erriquez, O.; Favuzzi, C.; Giglietto, N.; Nappi, E.; Spinelli, P.; Cecchini, S.; D'Antone, I.; Giacomelli, G.; Mandrioli, G.; Margiotta-Neri, A.; Matteuzzi, P.; Pal, B.; Patrizii, L.; Predieri, F.; Sanzani, G.L.; Serra, P.; Spurio, M.; Ahlen, S.P.; Ficenec, D.; Hazen, E.; Klein, S.; Levin, D.; Marin, A.; Stone, J.L.; Sulak, L.R.; Worstell, W.; Barish, B.; Coutu, S.; Hong, J.T.; Liu, G

1989-01-01T23:59:59.000Z

2

Measurement of the decoherence function with the MACRO detector at Gran Sasso  

SciTech Connect

A measurement of the underground muon decoherence function has been performed using the multiple muon events collected by the MACRO detector at the Gran Sasso National Laboratory. A detector-independent analysis is presented for different zenith regions and rock depths; this allows direct comparison with any model of hadronic interactions. The measured decoherence function is compared with the predictions of a Monte Carlo simulation based on data taken by recent collider experiments.

Ahlen, S.; Ambrosio, M.; Antolini, R.; Auriemma, G.; Baldini, A.; Barbarino, G.C.; Barish, B.C.; Battistoni, G.; Bellotti, R.; Bemporad, C.; Bernardini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, D.; Campana, P.; Carboni, M.; Cecchini, S.; Cei, F.; Chiarella, V.; Chiera, C.; Cobis, A.; Cormack, R.; Corona, A.; Coutu, S.; DeCataldo, G.; Dekhussi, H.; DeMarzo, C.; De Vincenzi, M.; Di Credico, A.; Diehl, E.; Erriquez, O.; Favuzzi, C.; Ficenec, D.; Forti, C.; Foti, L.; Fusco, P.; Giacomelli, G.; Giannini, G.; Giglietto, N.; Giubellino, P.; Grassi, M.; Green, P.; Grillo, A.; Guarino, F.; Gustavino, C.; Habig, A.; Heinz, R.; Hong, J.T.; Iarocci, E.; Katsavounidis, E.; Kearns, E.; Klein, S.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Lee, C.; Levin, D.S.; Lipari, P.; Liu, G.; Liu, R.; Longo, M.J.; Ludlam, G.; Mancarella, G.; Mandrioli, G.; Margiotta-Neri, A.; Marin, A.; Marini, A.; Martello, D.; Marzari Chiesa, A.; Masera, M.; Matteuzzi, P.; Michae; (MACRO Collaboration)

1992-12-01T23:59:59.000Z

3

Vertical muon intensity measured with MACRO at the Gran Sasso laboratory  

Science Conference Proceedings (OSTI)

The vertical underground muon intensity has been measured in the slant depth range 3200--7000 hg cm{sup {minus}2} (standard rock) with the completed lower part of the MACRO detector at the Gran Sasso laboratory, using a large sample of data. These observations are used to compute the surface muon flux and the primary ``all-nucleon`` spectrum. An analysis of systematic uncertainties introduced by the interaction models in the atmosphere and the underground propagation of muons is presented. A comparison of our results with published data is also presented.

Ambrosio, M.; Antolini, R.; Auriemma, G.; Baker, R.; Baldini, A.; Barbarino, G.C.; Barish, B.C.; Battistoni, G.; Bellotti, R.; Bemporad, C.; Bernardini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bower, C.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, D.; Carboni, M.; Castellano, M.; Cecchini, S.; Cei, F.; Celio, P.; Chiarella, V.; Corona, A.; Coutu, S.; De Cataldo, G.; Dekhissi, H.; De Marzo, C.; De Mitri, I.; De Vincenzi, M.; Di Credico, A.; Erriquez, O.; Favuzzi, C.; Forti, C.; Fusco, P.; Giacomelli, G.; Giannini, G.; Giglietto, N.; Grassi, M.; Grillo, A.; Guarino, F.; Guarnaccia, P.; Gustavino, C.; Habig, A.; Hanson, K.; Hawthorne, A.; Heinz, R.; Hong, J.T.; Iarocci, E.; Katsavounidis, E.; Kearns, E.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Levin, D.S.; Lipari, P.; Liu, R.; Longley, N.P.; Longo, M.J.; Lu, Y.; Ludlam, G.; Mancarella, G.; Mandrioli, G.; Margiotta-Neri, A.; Marini, A.; Martello, D.; Marzari-Chiesa, A.; Mazziotta, M.N.; Michael, D.G.; Mikheyev, S.; Miller, L.; Mittelbrunn, M.; Monacelli, P.; Montaruli, T.; Monteno, M.; Mufson, S.; Musser, J.; Nicolo, D.; Nolty, R.; Okada, C.; Orth, C.; Osteria, G.; Palamara, O.; Parlati, S.; Patera, V.; Patrizii, L.; Pazzi, R.; Peck, C.W.; Petrera, S.; Pignatano, N.D.; Pistilli, P.; Popa, V.; Raino, A.; Reynoldson, J.; Ronga, F.; Sanzgiri, A.; Sartogo, F.; Satriano, C.; Satta, L.; Scapparone, E.; Scholberg, K.; Sciubba, A.; Serra-Lugaresi, P.; Severi, M.; Sitta, M.; Spinelli, P.; Spinetti, M.; Spurio, M.; Steinberg, R.; Stone, J.L.; Sulak, L.R.; Surdo, A.; Tarle, G.; Tassoni, F.; Togo, V.; Valente, V.; Walter, C.W.; Webb, R. [Dipartimento di Fisica dell`Universita di Bari and Istituto Nazionale di Fisica Nucleare, 70126 Bari (Italy)]|[Dipartimento di Fisica dell`Universita di Bologna and Istituto Nazionale di Fisica Nucleare, 40126 Bologna (Italy)]|[Physics Department, Boston University, Boston, Massachusetts 02215 (United States)]|[California Institute of Technology, Pasadena, California 91125 (United States)...

1995-10-01T23:59:59.000Z

4

Simultaneous observation of extensive air showers and deep-underground muons at the Gran Sasso Laboratory  

Science Conference Proceedings (OSTI)

Combined measurements of extensive air showers at the surface and high-energy muons deep underground have been initiated at the Gran Sasso Laboratory. The underground detector is the first supermodule of MACRO (area=140 m{sup 2}, depth=3100 m of water equivalent , {ital E}{sub {mu}}{gt}1.3 TeV) and the surface detector is the EAS-TOP array (altitude 2000 m above sea level, total enclosed area {ital A}{approximately}10{sup 5} m{sup 2}). We discuss the correlation technique, the comparison between the shower parameters as determined by the two detectors, and some of the characteristics of the reconstructed events.

Bellotti, R.; Cafagna, F.; Caliccio, M.; De Cataldo, G.; De Marzo, C.; Erriquez, O.; Favuzzi, C.; Giglietto, N.; Nappi, E.; Spinelli, P. (Istituto di Fisica dell'Universita di Bari, Via Amendola, Bari (Italy)); Cecchini, S.; Fabbri, M.; Giacomelli, G.; Mandrioli, G.; Matteuzzi, P.; Pal, B.; Patrizii, L.; Predieri, F.; Sanzani, G.L.; Serra, P.; Spurio, M. (Dipartimento di Fisica dell'Universita di Bologna, Via Irnerio 46, I-40126, Bologna (Italy)); Ahlen, S.; Ficenec, D.; Hazen, E.; Klein, S.; Levin, D.; Marin, A.; Stone, J.L.; Sulak, L.R.; Worstell, W. (Physics Department, Boston University, 590 Commonwealth Avenue, Boston, MA (USA)); Barish, B.; Coutu, S.; Hong, J.; Liu, G.; Peck, C.; Solie, D.; Steele, J. (California Institute of Technology, Pasadena, CA (USA)); Lane, C.; Steinberg, R. (Physics Department, Drexel University, Philadelphia, PA (USA)); Battistoni, G.; Bilokon, H.; Bloise, C.; Campana, P.; Chiarella, V.; Forti, C.; Grillo, A.; Iarocci, E.; Marini, A.; Patera, V.; Re; MACRO Collaboration

1990-09-01T23:59:59.000Z

5

Study of single muons with the Large Volume Detector at Gran Sasso Laboratory  

E-Print Network (OSTI)

The present study is based on the sample of about 3 mln single muons observed by LVD at underground Gran Sasso Laboratory during 36500 live hours from June 1992 to February 1998. We have measured the muon intensity at slant depths from 3 km w.e. to 20 km w.e. Most events are high energy downward muons produced by meson decay in the atmosphere. The analysis of these muons has revealed the power index of pion and kaon spectrum: 2.76 \\pm 0.05. The reminders are horizontal muons produced by the neutrino interactions in the rock surrounding LVD. The value of this flux is obtained. The results are compared with Monte Carlo simulations and the world data.

Aglietta, M; Antonioli, P; Badino, G; Bari, G; Basile, M; Berezinsky, Veniamin Sergeevich; Bersani, F; Bertaina, M; Bertoni, R; Bruni, G; Cara Romeo, G; Castagnoli, C; Castellina, A; Chiavassa, A; Chinellato, J A; Cifarelli, Luisa; Cindolo, F; Contin, A; Dadykin, V L; Dos Santos, L G; Enikeev, R I; Fulgione, W; Galeotti, P; Ghia, P; Giusti, P; Gómez, F; Granella, R; Grianti, F; Gurentsov, V I; Iacobucci, G; Inoue, N; Kemp, E; Khalchukov, F F; Korolkova, E V; Korchaguin, P V; Korchaguin, V B; Kudryavtsev, V A; Luvisetto, Marisa L; Malguin, A S; Massam, Thomas; Mengotti-Silva, N; Morello, C; Nania, R; Navarra, G; Periale, L; Pesci, A; Picchi, P; Pless, I A; Ryasny, V G; Ryazhskaya; Saavedra, O; Saitoh, K; Sartorelli, G; Selvi, M; Taborgna, N; Talochkin, P; Trinchero, G C; Tsuji, S; Turtelli, A; Vallania, P; Vernetto, S; Vigorito, C; Votano, L; Wada, T; Weinstein, R; Widgoff, M; Yakushev, V F; Yamamoto, I; Zatsepin, G T; Zichichi, A

2003-01-01T23:59:59.000Z

6

Search for double beta decay with HPGe detectors at the Gran Sasso underground laboratory  

E-Print Network (OSTI)

Neutrinoless double-beta decay is practically the only way to establish the Majorana nature of the neutrino mass and its decay rate provides a probe of an effective neutrino mass. Double beta experiments are long-running underground experiments with specific challenges concerning the background reduction and the long term stability. These problems are addressed in this work for the Heidelberg-Moscow (HdM), GENIUS Test Facility (TF) and GERDA experiments. The HdM experiment collected data with enriched 76Ge high purity (HPGe) detectors from 1990 to 2003. An improved analysis of HdM data is presented, exploiting new calibration and spectral shape measurements with the HdM detectors. GENIUS-TF was a test-facility that verified the feasibility of using bare germanium detectors in liquid nitrogen. The first year results of this experiment are discussed. The GERDA experiment has been designed to further increase the sensitivity by operating bare germanium detectors in a high purity cryogenic liquid, which simultaneously serves as a shielding against background and as a cooling media. In the preparatory stage of GERDA, an external background gamma flux measurement was done at the experimental site in the Hall A of the Gran Sasso laboratory. The characterization of the enriched detectors from the HdM and IGEX experiments was performed in the underground detector laboratory for the GERDA collaboration. Long term stability measurements of a bare HPGe detector in liquid argon were carried out. Based on these measurements, the first lower limit on the half-life of neutrinoless double electron capture of 36Ar was established to be 1.85*10^18 years at 68% C.L.

Oleg Chkvorets

2008-12-05T23:59:59.000Z

7

C2GT intercepting CERN neutrinos to Gran Sasso in the Gulf of Taranto to measure $\\theta_13$  

E-Print Network (OSTI)

Today's greatest challenge in accelerator-based neutrino physics is to measure the mixing angle \\thonethree\\ which is known to be much smaller than the solar mixing angle \\thonetwo\\ and the atmospheric mixing angle \\thtwothree . A non-zero value of the angle \\thonethree\\ is a prerequisite for observing CP violation in neutrino mixing. In this paper, we discuss a deep-sea neutrino experiment with 1.5~Mt fiducial target mass in the Gulf of Taranto with the prime objective of measuring \\thonethree. The detector is exposed to the CERN neutrino beam to Gran Sasso in off-axis geometry. Monochromatic muon-neutrinos of $\\approx 800$~MeV energy are the dominant beam component. Neutrinos are detected through quasi-elastic, charged-current reactions in sea water; electrons and muons are detected in a large-surface, ring-imaging Cherenkov detector. The profile of the seabed in the Gulf of Taranto allows for a moveable experiment at variable distances from CERN, starting at 1100 km. From the oscillatory pattern of the dis...

Ball, A E; Camilleri, L L; Catinaccio, A; Chelkov, G A; Dydak, F; Elagin, A; Frandsen, Poul Kjaer; Gostkin, M I; Grant, A; Guskov, A; Joram, C; Krumshtein, Z; Müller, H; Postema, H; Price, M; Rovelli, T; Schinzel, D; Séguinot, Jacques; Valenti, G; Voss, R; Wotschack, J; Zhemchugov, A S

2007-01-01T23:59:59.000Z

8

extinciones La gran extincin que hace 65.5 millones  

E-Print Network (OSTI)

mapadeanomalíasgravimétricas4 delaPenínsuladeYu- catán y el Golfo de méxico, realizado por Pemex; pero no fue sino hasta 1991

Keller, Gerta

9

Using decision trees to select the gran natical relation of a noun phrase  

E-Print Network (OSTI)

-copula)(Si) Grammatical Relation ///L (PN) Po so.Po PCPeI ,//'t, NPCPP. I ~! adjective(PP,) } ., .. I ~ PPcomplementof J

10

The present status of the LUNA facility at the underground Gran Sasso Laboratory  

Science Conference Proceedings (OSTI)

The LUNA collaboration has recently completed the study of the electron screening effect in the D ( 3 He

S. Zavatarelli; on behalf of LUNA Collaboration

2002-01-01T23:59:59.000Z

11

Fermilab Today  

NLE Websites -- All DOE Office Websites (Extended Search)

of Minnesota Duluth Left to right: Ryan Trogstad, Cody Rude, Rik Gran, Alec Habig, Jordan Heaton and Emily Draeger in the electronics laboratory at the University of Minnesota...

12

Aerogeneradores Canarios SA ACSA | Open Energy Information  

Open Energy Info (EERE)

Las Palmas de Gran Canaria, Spain Zip 35011 Sector Wind energy Product Manufacturer mini wind-turbines and wind farm developer References Aerogeneradores Canarios SA (ACSA)1...

13

Doble homenaje: A Calderón y A Jorge Guillén  

E-Print Network (OSTI)

de su muerte; y a Jorge Guillen, gran poeta de nuestroA Calderón humo humo Jorge Guillen De habere door, que sexa

Barcia, José Rubia

1981-01-01T23:59:59.000Z

14

Compare Híbridos Lado a Lado  

NLE Websites -- All DOE Office Websites (Extended Search)

Compare Hbridos Lado a Lado Quiero Comparar... Nuevos Hbridos Autos Pequeos Sedanes Familiares Sedanes de Lujo y Gran Lujo Camionetas Tipo Pickup Camionetas Deportivas Todo...

15

Híbridos Enchufables  

NLE Websites -- All DOE Office Websites (Extended Search)

Hbridos Enchufables Chevrolet Volt Vehculos Elctricos Enchufables (PHEVs) son hbridos con bateras de gran capacidad que pueden ser recargables conectndose a una caja de...

16

CERN  

NLE Websites -- All DOE Office Websites (Extended Search)

y nuevas partculas y fuerzas fundamentales. Para mayor informacin: LHC: Large Hadron Collider El gran colisionador de hadrones se ha planeado que habite en el mismo tnel...

17

Inquiring Minds  

NLE Websites -- All DOE Office Websites (Extended Search)

by Gran Sasso and Heidelberg to operate Ge detectors in liquid nitrogen. GLAST: Gamma-ray Large Area Space Telescope. A proposed orbiting telescope for high-energy gamma rays....

18

Ground-Source Heat Pumps for Domestic and Commercial Applications...  

NLE Websites -- All DOE Office Websites (Extended Search)

Ground-Source Heat Pumps for Domestic and Commercial Applications in Europe Speaker(s): Gran Hellstrm Date: May 2, 2006 - 12:00pm Location: Bldg. 90 Seminar HostPoint of...

19

The Granular Sea Ice Model in Spherical Coordinates and Its Application to a Global Climate Model  

Science Conference Proceedings (OSTI)

The granular sea ice model (GRAN) from Tremblay and Mysak is converted from Cartesian to spherical coordinates. In this conversion, the metric terms in the divergence of the deviatoric stress and in the strain rates are included. As an ...

Jan Sedlacek; Jean-François Lemieux; Lawrence A. Mysak; L. Bruno Tremblay; David M. Holland

2007-12-01T23:59:59.000Z

20

Coincident observation of air [hacek C]erenkov light by a surface array and muon bundles by a deep underground detector  

Science Conference Proceedings (OSTI)

We report on the simultaneous observation of atmospheric [hacek C]erenkov light by a prototype five telescope array, GRACE, (Gran Sasso Air [hacek C]erenkov Experiment) with deep underground muons in the MACRO (Monopole Astrophysics and Cosmic Ray Observatory). The telescope array was deployed at Campo Imperatore above the Gran Sasso Laboratory for a run completed in the fall of 1992. The total live time for the combined surface-underground operation was [similar to]100 h during which more than 300 events were seen in coincidence. The efficacy of this technique to monitor the electromagnetic and penetrating muon components of a cosmic-ray-induced cascade is discussed.

Ambrosio, M.; Antolini, R.; Auriemma, G.; Baker, R.; Baldini, A.; Bam, B.; Barbarino, G.C.; Barish, B.C.; Battistoni, G.; Bellotti, R.; Bemporad, C.; Bernardini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bower, C.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, D.; Carboni, M.; Corona, A.; Cecchini, S.; Cei, F.; Chiarella, V.; Cormack, R.; Coutu, S.; DeCataldo, G.; Dekhissi, H.; DeMarzo, C.; De Vincenzi, M.; Di Credico, A.; Diehl, E.; Erriquez, O.; Favuzzi, C.; Forti, C.; Fusco, P.; Giacomelli, G.; Giannini, G.; Giglietto, N.; Grassi, M.; Green, P.; Grillo, A.; Guarino, F.; Guarnaccia, P.; Gustavino, C.; Habig, A.; Heinz, R.; Hong, J.T.; Iarocci, E.; Katsavounidis, E.; Kearns, E.; Kertzman, M.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Lee, C.; Levin, D.S.; Lipari, P.; Liu, G.; Liu, R.; Longo, M.J.; Lu, Y.; Ludlam, G.; Mancarella, G.; Mandrioli, G.; Margiotta-Neri, A.; Marin, A.; Marini, A.; Martello, D.; Marzari Chiesa, A.; Michael, D.G.; Mikheyev, S.; Miller, L.; Mittlebrunn, M.; Mon; (GRACE and MACRO Collaborations)

1994-09-01T23:59:59.000Z

Note: This page contains sample records for the topic "idgeport-prunt ytown gran" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


21

Windows beyond the Standard Model  

SciTech Connect

DAMA is an observatory for rare processes at the Gran Sasso National Laboratory of the I.N.F.N. (LNGS). Here some arguments will be shortly summarised on the investigation on dark matter (DM) particles by annual modulation signature and on some of the performed searches for double beta decay modes.

Bernabei, R. [Dip. di Fisica, Universita di Roma 'Tor Vergata' and INFN-Roma Tor Vergata, 00133 Rome (Italy)

2007-10-12T23:59:59.000Z

22

CATEGORIAL GRAMMARS FOR STRATA OF NON-CF LANGUAGES AND THEIR PARSERS Michal P. Chy'til Hans Karlgren  

E-Print Network (OSTI)

to apply next~ the eategorial parser must m~ke an intelligen~ choice out of a list of alternative oate- n hoe and heuristic teelmiques? If. Proposed solution We introduce in nontechnical langn/- a~'e the essence of the proposed generaliza- tion of eategorial gran.nars ~d their parsers. Tile exact mathematical

23

Grand Unified Theory  

NLE Websites -- All DOE Office Websites (Extended Search)

de la Gran Unificación de la Gran Unificación Volver Principal ESTOY PERDIDO!!! La teoría que (¡esperamos!) unificará las interacciones fuerte, débil, y electromagnética, es la llamada "Teoría de Gran Unificación (TGU)." Los físicos pueden escribir acerca de estas teorías hoy en día, pero se necesitan aún más datos para decir cuál de las muchas versiones describe la naturaleza, si es que alguna lo hace. Suponiendo que sea posible una Gran Unificación de todas las interacciones, entonces todas las interacciones que observamos no son más que diferentes aspectos de la misma teoría unificada. Sin embargo, ¿cómo puede éste ser el caso, cuando las interacciones fuerte, débil y electromagnética son tan diferentes en intensidad y efecto? Aunque parezca

24

The GERDA experiment for the search of 0??? decay in ^{76}Ge  

E-Print Network (OSTI)

The GERDA collaboration is performing a search for neutrinoless double beta decay of ^{76}Ge with the eponymous detector. The experiment has been installed and commissioned at the Laboratori Nazionali del Gran Sasso and has started operation in November 2011. The design, construction and first operational results are described, along with detailed information from the R&D phase.

GERDA Collaboration; K. -H. Ackermann; M. Agostini; M. Allardt; M. Altmann; E. Andreotti; A. M. Bakalyarov; M. Balata; I. Barabanov; M. Barnabe Heider; N. Barros; L. Baudis; C. Bauer; N. Becerici-Schmidt; E. Bellotti; S. Belogurov; S. T. Belyaev; G. Benato; A. Bettini; L. Bezrukov; T. Bode; V. Brudanin; R. Brugnera; D. Budjas; A. Caldwell; C. Cattadori; A. Chernogorov; O. Chkvorets; F. Cossavella; A. D`Andragora; E. V. Demidova; A. Denisov; A. di Vacri; A. Domula; V. Egorov; R. Falkenstein; A. Ferella; K. Freund; F. Froborg; N. Frodyma; A. Gangapshev; A. Garfagnini; J. Gasparro; S. Gazzana; R. Gonzalez de Orduna; P. Grabmayr; V. Gurentsov; K. Gusev; K. K. Guthikonda; W. Hampel; A. Hegai; M. Heisel; S. Hemmer; G. Heusser; W. Hofmann; M. Hult; L. V. Inzhechik; L. Ioannucci; J. Janicsko Csalty; J. Jochum; M. Junker; R. Kankanyan; S. Kianovsky; T. Kihm; J. Kiko; I. V. Kirpichnikov; A. Kirsch; A. Klimenko; M. Knapp; K. T. Knöpfle; O. Kochetov; V. N. Kornoukhov; K. Kröninger; V. Kusminov; M. Laubenstein; A. Lazzaro; V. I. Lebedev; B. Lehnert; D. Lenz; H. Liao; M. Lindner; I. Lippi; J. Liu; X. Liu; A. Lubashevskiy; B. Lubsandorzhiev; A. A. Machado; B. Majorovits; W. Maneschg; G. Marissens; S. Mayer; G. Meierhofer; I. Nemchenok; L. Niedermeier; S. Nisi; J. Oehm; C. O'Shaughnessy; L. Pandola; P. Peiffer; K. Pelczar; A. Pullia; S. Riboldi; F. Ritter; C. Rossi Alvarez; C. Sada; M. Salathe; C. Schmitt; S. Schönert; J. Schreiner; J. Schubert; O. Schulz; U. Schwan; B. Schwingenheuer; H. Seitz; E. Shevchik; M. Shirchenko; H. Simgen; A. Smolnikov; L. Stanco; F. Stelzer; H. Strecker; M. Tarka; U. Trunk; C. A. Ur; A. A. Vasenko; S. Vogt; O. Volynets; K. von Sturm; V. Wagner; M. Walter; A. Wegmann; M. Wojcik; E. Yanovich; P. Zavarise; I. Zhitnikov; S. V. Zhukov; D. Zinatulina; K. Zuber; G. Zuzel

2012-12-17T23:59:59.000Z

25

Search for a Possible Spontaneous Emission of Muons from Heavy Nuclei  

E-Print Network (OSTI)

A search for an exotic natural radioactivity of lead nuclei, using nuclear emulsion sheets as detector, is described. We discuss the experimental set-up of a test performed at the Gran Sasso National Laboratory (Italy), the event simulation, data analysis and preliminary results.

M. Giorgini

2010-01-21T23:59:59.000Z

26

Study of CR primaries and their cascades at E0 = 10-100 TeV through EAS-TOP and MACRO  

E-Print Network (OSTI)

A measurement of the lateral distribution of Cherenkov light in Extensive Air Showers (EAS) at E0 = 10-100 TeV and a study of the compatibility of the photon number spectra with the expectations from the direct measurements of p and He spectra and the Corsika-QGSJET propagation code in the atmosphere have been performed at the National Gran Sasso Laboratories by the EAS-TOP and MACRO arrays. The telescope array of EAS-TOP has been used as the Cherenkov light detector. The muon tracking system of MACRO in the deep underground Gran Sasso Laboratories (Emuon> 1.3 TeV) served as the EAS detector, including core localization and arrival direction.

The EAS-TOP; MACRO Collaborations

2001-12-20T23:59:59.000Z

27

The XENON100 Dark Matter Experiment  

SciTech Connect

The XENON100 experiment is searching for WIMPs, which are particles that may consist dark matter. It is located in the underground laboratory of Gran Sasso (LNGS) in Italy at a depth of {approx}3600 m.w.e.. The experiment description, its performance and the expected background based on Monte Carlo simulations and material screening along with the projected sensitivities of the experiment are presented. In addition, a brief description of the upgrade XENON100 detector is given.

Tziaferi, E. [Physics Institute, University of Zuerich, Winterthurerstr. 190, Zuerich (Switzerland)

2010-06-23T23:59:59.000Z

28

Weaver, P.P.E., Schmincke, H.-U., Firth, J.V., and Duffield, W. (Eds.), 1998 Proceedings of the Ocean Drilling Program, Scientific Results, Vol. 157  

E-Print Network (OSTI)

­PLEISTOCENE FALLOUT TEPHRA LAYERS AND VOLCANICLASTIC DEPOSITS IN THE SEDIMENTARY APRONS OF GRAN CANARIA AND TENERIFE (SITES 953, 954, AND 956)1 Paul van den Bogaard2 ABSTRACT Six fallout tephra layers and 16. The fallout tephra markers range in age from 0.273 ± 0.006 Ma to 2.74 ± 0.01 Ma. Maximum sedimentation ages

29

Captulo 15 Gas ideal de fermiones.  

E-Print Network (OSTI)

mediante el aumento de la fracci´on de ionizaci´on del hidr´ogeno a medida que se calienta de 5000 a 8000 gran tama~no de las cromosferas de las estrellas de tipo solar. Una vez que el hidr´ogeno se encuentra. 2010). Las l´ineas de la serie de Balmer del hidr´ogeno tambi´en se ven afectadas por la actividad magn

Colet, Pere

30

Study of solar and other unknown anti-neutrino fluxes with Borexino at LNGS  

E-Print Network (OSTI)

We report on the search for anti-neutrinos of yet unknown origin with the Borexino detector at the Laboratori Nazionali del Gran Sasso. In particular, a hypothetical anti-neutrino flux from the Sun is investigated. Anti-neutrinos are detected through the neutron inverse $\\beta$ decay reaction in a large liquid organic scintillator target. We set a new upper limit for a hypothetical solar $\\bar{\

G. Bellini; Borexino Collaboration

2010-09-30T23:59:59.000Z

31

Indiana University High Energy Physics Group, Task C  

Science Conference Proceedings (OSTI)

The Indiana University High Energy Physics Group, Task C has been actively involved in the MACRO experiment at Gran Sasso and the SSC experiment L during the current contract year. MACRO is a large US-Italian Monopole, Astrophysics, and Cosmic Ray Observatory being built under the Gran Sasso Mountain outside of Rome. Indiana University is in charge of organizing the United States software effort. We have built a state-of-the-art two-meter spectrophotometer for the MACRO liquid scintillator. We are in charge of ERP, the Event Reconstruction Processor online trigger processor for muons and stellar collapse. We are designing an air Cerenkov array to be placed on top of the Gran Sasso. Our other activity involves participation in the SSC experiment L. As long-standing members of L we have done proposal writing and have worked on important L planning and organization matters. We are now doing development work on the L Central Tracker straw drift tubes, including gas optimization, readout, and Monte Carlos. 12 refs., 20 figs., 1 tab.

Heinz, R.M.; Mufson, S.L.; Musser, J.

1991-01-01T23:59:59.000Z

32

ICARUS and Status of Liquid Argon Technology  

E-Print Network (OSTI)

ICARUS is the largest liquid argon TPC detector ever built (~600 ton LAr mass). It operates underground at the LNGS laboratory in Gran Sasso. It has been smoothly running since summer 2010, collecting data with the CNGS beam and with cosmics. Liquid argon TPCs are really "electronic bubble chamber" providing a completely uniform imaging and calorimetry with unprecedented accuracy on massive volumes. ICARUS is internationally considered as a milestone towards the realization of the next generation of massive detectors (~tens of ktons) for neutrino and rare event physics. Results will be presented on the data collected during 2010 with the detector at LNGS.

Dorota Stefan

2011-10-07T23:59:59.000Z

33

Search for massive rare particles with MACRO  

E-Print Network (OSTI)

Massive rare particles have been searched for in the penetrating cosmic radiation using the MACRO apparatus at the Gran Sasso National Laboratories. Liquid scintillators, streamer tubes and nuclear track detectors have been used to search for magnetic monopoles (MMs). Based on no observation of such signals, stringent flux limits are established for MMs as slow as a few 10^(-5)c. The methods based on the scintillator and on the nuclear track subdetectors were also applied to search for nuclearites. Preliminary results of the searches for charged Q-balls are also presented.

The MACRO Collaboration

2000-09-01T23:59:59.000Z

34

On-line recognition of supernova neutrino bursts in the LVD detector  

E-Print Network (OSTI)

In this paper we show the capabilities of the Large Volume Detector (INFN Gran Sasso National Laboratory) to identify a neutrino burst associated to a supernova explosion, in the absence of an "external trigger", e.g., an optical observation. We describe how the detector trigger and event selection have been optimized for this purpose, and we detail the algorithm used for the on-line burst recognition. The on-line sensitivity of the detector is defined and discussed in terms of supernova distance and electron anti-neutrino intensity at the source.

N. Yu. Agafonova; M. Aglietta; P. Antonioli; G. Bari; A. Bonardi; V. V. Boyarkin; G. Bruno; W. Fulgione; P. Galeotti; M. Garbini; P. L. Ghia; P. Giusti; F. Gomez; E. Kemp; V. V. Kuznetsov; V. A. Kuznetsov; A. S. Malguin; H. Menghetti; A. Pesci; R. Persiani; I. A. Pless; A. Porta; V. G. Ryasny; O. G. Ryazhskaya; O. Saavedra; G. Sartorelli; M. Selvi; C. Vigorito; L. Votano; V. F. Yakushev; G. T. Zatsepin; A. Zichichi

2007-10-01T23:59:59.000Z

35

Does OPERA probe that the Earth is moving ?  

E-Print Network (OSTI)

The OPERA experiment reported recently a puzzling result. The time of flight of a neutrino beam between the CERN and the Gran Sasso Laboratory has been measured to be slightly shorter than expected. More precisely, an early arrival time of the neutrino with respect to the one computed assuming the speed of light in vacuum of 60.7 ns was measured, with a quite high confidence level. Alternatively, one can conclude that the neutrinos travelled 18.2 m more than light would do in vacuum. In this short paper, we suggest a possible systematic effect that does not appear in the analysis and which can easily been probed to be confirmed.

Dominique Monderen

2011-10-17T23:59:59.000Z

36

Los linajes de transmision de Nyag bla Padma bdud'dul  

E-Print Network (OSTI)

tradición a los que hetenido acceso. Entre los lamas más reconocidos de la transmisión de Padma bdud ’dul(tanto en el papel de maestros como de discípulos) hay que destacar mDomkhyen brtse Ye shes rdo rje, Mi ’gyur nam mkha’i rdo rje, rDza dPal sprulRin po... importantes, tanto por la singularidad de estos personajes —posesores de un gran carisma en la orden rNying ma pa — como por lasenseñanzas y consejos que dieron al joven yogui. Mi ’gyur nam mkha’ rdo rje (1793-?), cuarta encarnación de rDzogs chenPadma rig...

Aguillar, Oriol

2005-01-01T23:59:59.000Z

37

 

NLE Websites -- All DOE Office Websites (Extended Search)

Stellar Fusion Cross Sections Underground Stellar Fusion Cross Sections Underground Daniel Bemmerer Forschungszentrum Dresden-Rossendorf (FZD) Abstract: Due to the suppression by the Coulomb barrier, the cross sections of astrophysically relevant nuclear reactions are very low at the stellar energy. Therefore they can only be directly measured in a low-background environment. For more than a decade now, the LUNA collaboration has pursued this approach with a 0.4 MV accelerator in the Gran Sasso underground laboratory in Italy. It was highly successful in studying the nuclear physics of the Sun and of the Big Bang. However, the energy range of LUNA is not sufficient to address the nuclear reactions of stellar helium and carbon burning and the neutron source reactions for the astrophysical s-process. Therefore, in the 2010 NuPECC

38

u.s. DEPARTMENT OFENER Y I EERE PROJECT MANAGEMENT C NTER NEPADETERMINATION  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

p ... .t!) p ... .t!) u.s. DEPARTMENT OFENER Y I EERE PROJECT MANAGEMENT C NTER NEPADETERMINATION RECIPIE"'T:State of Hawaii, DBEDT - SID STATE: HI PROJECT TITLE: State Energy Program, Program Year 2012 Formula Gran 5 Funding Opportunity Announcement Number Procurement Instrument N mber NEPA Control Number CID Number EEOO03928 I GFO-OOO3928-002 Based on my review orlhe information concerning the proposed action, as NEP Compliance Officer (authorized under DOE Order 451.1A), I have made the following determination: ex, EA, EIS APPENDIX AND NUMBER: Description: A9 Info rmation gathering, analysis, and d issemination A11 Technical advice and assistance to o rg anizations Rational for determination: Information gathering (including, but not limited to, lite ature surveys, inventories, site visits, and

39

Gas Natural - CNG y GNL  

NLE Websites -- All DOE Office Websites (Extended Search)

Gas Natural Dispensador de Gas Natural Gas Natural Dispensador de Gas Natural El gas natural, un combustible fósil compuesto básicamente de metano, es uno de los combustibles alternativos menos contaminantes. Puede ser usado como gas natural comprimido (GNC) o como gas natural licuado (GNL) para autos y camiones. Existen vehículos diseñados para funcionar exclusivamente con gas natural. Por otra parte hay vehículos de doble combustible o bi-combustibles que también puede funcionar con gasolina o diesel. Los vehículos de doble combustible permiten que el usuario aproveche la gran disponibilidad de gasolina o diesel, pero use la alternativa menos contaminante y más económica cuando el gas natural esté disponible. Ya que el gas natural es almacenado en depósitos de combustible de alta

40

 

NLE Websites -- All DOE Office Websites (Extended Search)

VOGEL/PIEP on 02-Jan-2014 VOGEL/PIEP on 02-Jan-2014 Status Dates: 08/01/2013 to 12/31/2013 Status Flags are: UNRELEASED, RELEASED, ASSIGNED, ENCODED, OVERSEEN, ACCEPTED, VERIFIED, PUBLISHED Contents Modes are: UNKNOWN, DATA, EMPTY Publication Modes are: NEW, PUBLISHED Click on the journal reference to find article in INSPIRE. Make sure to use the journal, as opposed to arXiv, version for encoding. INSPIRE link EPJ A49 24 BELLI 13 LIN S076 Double-beta D$ released unknown new VOGEL/PIEP 10/02/2013 HPGe; GranSAS$ EPJ C73 2323 KRAUS 13 LIN S077 NUCL Heavy-Neutral$ released unknown new VOGEL/PIEP 10/02/2013 sterile nu EPJ C73 2330 ACKERMANN 13 LIN S076 Double-beta D$ released unknown new VOGEL/PIEP 10/02/2013 GERDA EPJ C73 2345 ANTONELLO 13 LIN S067 NUCL Neutrino Mixi$

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41

Experimental study of double-{beta} decay modes using a CdZnTe detector array  

SciTech Connect

An array of sixteen 1 cm{sup 3} CdZnTe semiconductor detectors was operated at the Gran Sasso Underground Laboratory (LNGS) to further investigate the feasibility of double-{beta} decay searches with such devices. As one of the double-{beta} decay experiments with the highest granularity the 4x4 array accumulated an overall exposure of 18 kg days. The setup and performance of the array is described. Half-life limits for various double-{beta} decay modes of Cd, Zn, and Te isotopes are obtained. No signal has been found, but several limits beyond 10{sup 20} years have been performed. They are an order of magnitude better than those obtained with this technology before and comparable to most other experimental approaches for the isotopes under investigation. An improved limit for the {beta}{sup +}/EC decay of {sup 120}Te is given.

Dawson, J. V. [Laboratoire Astroparticule et Cosmologie, 10 rue Alice Domon et Leonie Duquet, F-75205 Paris (France); Goessling, C.; Koettig, T.; Muenstermann, D.; Rajek, S.; Schulz, O. [Lehrstuhl fuer Experimentelle Physik IV, Technische Universitaet Dortmund, Otto-Hahn Str. 4, D-44227 Dortmund (Germany); Janutta, B.; Zuber, K. [Institut fuer Kern- und Teilchenphysik, Technische Universitaet Dresden, Zellescher Weg 19, D-01069 Dresden (Germany); Junker, M. [Laboratori Nazionali del Gran Sasso, Assergi (Italy); Reeve, C. [University of Sussex, Falmer, Brighton BN1 9QH (United Kingdom); Wilson, J. R. [University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH (United Kingdom)

2009-08-15T23:59:59.000Z

42

Información de Recursos ERNC | Open Energy Information  

Open Energy Info (EERE)

Información de Recursos ERNC Información de Recursos ERNC Jump to: navigation, search Información General Geospatial Toolkits Esta herramienta fue desarrollada por NREL para realizar evaluaciones integradas de recursos renovables. Al usar gran cantidad de datos, genera mapas de alta resolución que pueden ser integrados en softwares como HOMER, para obtener modelos de generación de energía. Map Search Map Search es una base de datos de NREL que contiene mapas de recursos naturales para todos los países Latinoaméricanos, especificamente de recursos solares y eólicos. REN21 Mapa Interactivo de Energías Renovables Mapa interactivo que muestra información sobre políticas de energías renovables en diferentes países, capacidad instalada y otros datos relacionados. Aunque el mapa no es una fuente de datos directa de recursos

43

validation | OpenEI  

Open Energy Info (EERE)

validation validation Dataset Summary Description (Abstract): 31Conclusiones y recomendacionesEl método de cálculo de la radiación solar global desarrollado ha obtenido resultadoscomparables a otros métodos revisados en la bibliografía. A diferencia de muchos deestos métodos, que han sido ajustados y refinados por sus autores a lo largo de variosaños de trabajo, este es completamente nuevo y parte de un enfoque diferente, por loque tiene un gran potencial de ajuste y sintonización.Algunos cambios que pueden sugerirse son tomar distribuciones espaciales ytemporales Source Instituto de Meteorología de Cuba Date Released November 30th, 2005 (9 years ago) Date Updated November 07th, 2007 (7 years ago) Keywords América Latina Cuba documentation solar SWERA validation

44

Study of the ultrahigh-energy primary-cosmic-ray composition with the MACRO experiment  

Science Conference Proceedings (OSTI)

We present the analysis of multiple-muon events collected with one supermodule (1013 h live time) and two supermodules (1195 h live time) of the MACRO detector at Gran Sasso, Italy. Multimuon rates are shown to be sensitive to primary-cosmic-ray energies between {similar to}50 TeV and several thousand TeV. Experimental data are compared with the expected rates from two composition models: a light (i.e., proton-rich) and a heavy (i.e., Fe-rich) composition. The predictions are based on a Monte Carlo simulation of the hadronic interactions of cosmic-ray nuclei, followed by a detailed tracking of the muons through the rock and the experimental apparatus. The results show good sensitivity of the MACRO detector to primary composition. The data exhibit a preference towards the light composition model.

Ahlen, S.; Ambrosio, M.; Antolini, R.; Auriemma, G.; Baldini, A.; Bam, B.B.; Barbarino, G.C.; Barish, B.C.; Battistoni, G.; Bellotti, R.; Bemporad, C.; Bernardini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, P.; Campana, D.; Carboni, M.; Cecchini, S.; Cei, F.; Chiarella, V.; Chiera, C.; Cobis, A.; Cormack, R.; Corona, A.; Coutu, S.; DeCataldo, G.; DeMarzo, C.; De Vincenzi, M.; Di Credico, A.; Diehl, E.; Erriquez, O.; Favuzzi, C.; Ficenec, D.; Forti, C.; Foti, L.; Fusco, P.; Giacomelli, G.; Giannini, G.; Giglietto, N.; Giubellino, P.; Grassi, M.; Green, P.; Grillo, A.; Guarino, F.; Gustavino, C.; Habig, A.; Heinz, R.; Hong, J.T.; Iarocci, E.; Katsavounidis, E.; Kearns, E.; Klein, S.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Lee, C.; Levin, D.; Lipari, P.; Liu, G.; Liu, R.; Longo, M.J.; Ludlam, G.; Mancarella, G.; Mandrioli, G.; Margiotta-Neri, A.; Marin, A.; Marini, A.; Martello, D.; Martellotti, G.; Marzari Chiesa, A.; Masera, M.; Matteuzzi; (MACRO Collaboration)

1992-08-01T23:59:59.000Z

45

Search for slowly moving magnetic monopoles with the MACRO detector  

Science Conference Proceedings (OSTI)

A search for slowly moving magnetic monopoles in the cosmic radiation was conducted from October 1989 to November 1991 using the large liquid scintillator detector subsystem of the first supermodule of the MACRO detector at the Gran Sasso underground laboratory. The absence of candidates established an upper limit on the monopole flux of 5.6[times]10[sup [minus]15] cm[sup [minus]2] sr[sup [minus]1] s[sup [minus]1] at 90% confidence level in the velocity range of 10[sup [minus]4][approx lt][beta][lt]4[times]10[sup [minus]3]. This result places a new constraint on the abundance of monopoles trapped in our solar system.

Ahlen, S.; Ambrosio, M.; Antolini, R.; Auriemma, G.; Baker, R.; Baldini, A.; Bam, B.B.; Barbarino, G.C.; Barish, B.C.; Battistoni, G.; Bellotti, R.; Bemporad, C.; Bernandini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bower, C.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, D.; Campana, P.; Carboni, M.; Cecchini, S.; Cei, F.; Chiarella, V.; Cormack, R.; Corona, A.; Coutu, S.; De Cataldo, G.; Dekhissi, H.; De Marzo, C.; De Vincenzi, M.; Di Credico, A.; Diehl, E.; Erriquez, O.; Favuzzi, C.; Ficenec, D.; Forti, C.; Fusco, P.; Giacomelli, G.; Giannini, G.; Giglietto, N.; Giubellino, P.; Grassi, M.; Green, P.; Grillo, A.; Guarino, F.; Guarnaccia, P.; Gustavino, C.; Habig, A.; Heinz, R.; Hong, J.T.; Iarocci, E.; Katsavounidis, E.; Kearns, E.; Klein, S.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Lee, C.; Levin, D.; Lipari, P.; Liu, G.; Liu, R.; Longo, M.J.; Lu, Y.; Ludlam, G.; Mancarella, G.; Mandrioli, G.; Margiotta-Neri, A.; Marin, A.; Marini, A.; Martello, D.; Marzari Chiesa, A.; Masera, M; (MACRO Collaboration)

1994-01-31T23:59:59.000Z

46

Ventilation and air-conditioning concept for CNGS underground areas  

E-Print Network (OSTI)

The aim of the CNGS project is to prove the existence of neutrino oscillation by generating an intense neutrino beam from CERN in the direction of the Gran Sasso laboratory in Italy, where two large neutrino detectors are built to detect the neutrinos. All the components for producing the neutrino beam will be situated in the underground tunnels, service galleries and chambers. The ventilation and air-conditioning systems installed in these underground areas have multiple tasks. Depending on the operating mode and structure to be air-conditioned, the systems are required to provide fresh air, cool the machine, dehumidify areas housing sensible equipment or assure the smoke removal in a case of a fire. This paper presents the technical solutions foreseen to meet these requirements.

Lindroos, J

2002-01-01T23:59:59.000Z

47

Science and Technology of BOREXINO: A Real Time Detector for Low Energy Solar Neutrinos SOLAR NEUTRINOS  

E-Print Network (OSTI)

BOREXINO, a real-time device for low energy neutrino spectroscopy is nearing completion of construction in the underground laboratories at Gran Sasso, Italy (LNGS). The experiment's goal is the direct measurement of the flux of 7Be solar neutrinos of all flavors via neutrino-electron scattering in an ultra-pure scintillation liquid. Seeded by a series of innovations which were brought to fruition by large scale operation of a 4-ton test detector at LNGS, a new technology has been developed for BOREXINO. It enables sub-MeV solar neutrino spectroscopy for the first time. This paper describes the design of BOREXINO, the various facilities essential to its operation, its spectroscopic and background suppression capabilities and a prognosis of the impact of its results towards resolving the solar neutrino problem. BOREXINO will also address several other frontier questions in particle physics, astrophysics and geophysics.

Borexino Collaboration; G. Alimonti

2000-12-11T23:59:59.000Z

48

The 3He(alpha,gamma)7Be S-factor at solar energies: the prompt gamma experiment at LUNA  

E-Print Network (OSTI)

The 3He(alpha,gamma)7Be process is a key reaction in both Big-Bang nucleosynthesis and p-p chain of Hydrogen Burning in Stars. A new measurement of the 3He(alpha,gamma)7Be cross section has been performed at the INFN Gran Sasso underground laboratory by both the activation and the prompt gamma detection methods. The present work reports full details of the prompt gamma detection experiment, focusing on the determination of the systematic uncertainty. The final data, including activation measurements at LUNA, are compared with the results of the last generation experiments and two different theoretical models are used to obtain the S-factor at solar energies.

H. Costantini; D. Bemmerer; F. Confortola; A. Formicola; Gy. Gyürky; P. Bezzon; R. Bonetti; C. Broggini; P. Corvisiero; Z. Elekes; Zs. Fülöp; G. Gervino; A. Guglielmetti; C. Gustavino; G. Imbriani; M. Junker; M. Laubenstein; A. Lemut; B. Limata; V. Lozza; M. Marta; R. Menegazzo; P. Prati; V. Roca; C. Rolfs; C. Rossi Alvarez; E. Somorjai; O. Straniero; F. Strieder; F. Terrasi; H. P. Trautvetter

2008-09-30T23:59:59.000Z

49

Borexino: A real time liquid scintillator detector for low energy solar neutrino study  

E-Print Network (OSTI)

Borexino is a large unsegmented calorimeter featuring 300 tons of liquid scintillator, contained in a 8.5 meter nylon vessel, viewed by 2200 PMTs. The main goal of Borexino is the study, in real time, of low energy solar neutrinos, and in particular, the monoenergetic neutrinos coming from $^7Be$, which is one of the missing links on the solar neutrino problem. The achievement of high radiopurity level, in the order of $10^{-16} g/g$ of U/Th equivalent, necessary to the detection of the low energy component of the solar neutrino flux, was proved in the Borexino prototype: the Counting Test Facility. The detector is located underground in the Laboratori Nazionali del Gran Sasso in the center of Italy at 3500 meter water equivalent depth. In this paper the science and technology of Borexino are reviewed and its main capabilities are presented.

Lino Miramonti

2002-06-25T23:59:59.000Z

50

The Cross Section of 3He(3He,2p)4He measured at Solar Energies  

E-Print Network (OSTI)

We report on the results of the \\hethet\\ experiment at the underground accelerator facility LUNA (Gran Sasso). For the first time the lowest projectile energies utilized for the cross section measurement correspond to energies below the center of the solar Gamow peak ($E_{\\rm 0}$=22 keV). The data provide no evidence for the existence of a hypothetical resonance in the energy range investigated. Although no extrapolation is needed anymore (except for energies at the low-energy tail of the Gamow peak), the data must be corrected for the effects of electron screening, clearly observed the first time for the \\hethet\\ reaction. The effects are however larger than expected and not understood, leading presently to the largest uncertainty on the quoted $S_{\\rm b}(E_{\\rm 0})$ value for bare nuclides (=5.40 MeV b).

The LUNA Collaboration; M. Junker; A. D'Alessandro; S. Zavatarelli; C. Arpesella; E. Bellotti; C. Broggini; P. Corvisiero; G. Fiorentini; A. Fubini; G. Gervino; U. Greife; C. Gustavino; J. Lambert; P. Prati; W. S. Rodney; C. Rolfs; F. Strieder; H. P. Trautvetter; D. Zahnow

1997-07-10T23:59:59.000Z

51

Search for double beta decay of Zinc and Tungsten with the help of low-background ZnWO4 crystal scintillators  

E-Print Network (OSTI)

Double beta processes in 64-Zn, 70-Zn, 180-W, and 186-W have been searched for with the help of large volume (0.1-0.7 kg) low background ZnWO4 crystal scintillators at the Gran Sasso National Laboratories of the INFN. Total time of measurements exceeds 10 thousands hours. New improved half-life limits on double electron capture and electron capture with positron emission in 64-Zn have been set, in particular (all the limits are at 90% C.L.): T1/2(0nu2EC)> 1.1e20 yr, T1/2(2nuECbeta+)>7.0e20 yr, and T1/2(0nuECbeta+)>4.3e20 yr. The different modes of double beta processes in 70-Zn, 180-W, and 186-W have been restricted at the level of 1e17-1e20 yr.

P. Belli; R. Bernabei; F. Cappella; R. Cerulli; F. A. Danevich; B. V. Grinyov; A. Incicchitti; V. V. Kobychev; V. M. Mokina; S. S. Nagorny; L. L. Nagornaya; S. Nisi; F. Nozzoli; D. V. Poda; D. Prosperi; V. I. Tretyak; S. S. Yurchenko

2008-11-14T23:59:59.000Z

52

Performance of a large TeO2 crystal as a cryogenic bolometer in searching for neutrinoless double beta decay  

E-Print Network (OSTI)

Bolometers are ideal devices in the search for neutrinoless Double Beta Decay. Enlarging the mass of individual detectors would simplify the construction of a large experiment, but would also decrease the background per unit mass induced by alpha-emitters located close to the surfaces and background arising from external and internal gamma's. We present the very promising results obtained with a 2.13 kg TeO2 crystal. This bolometer, cooled down to a temperature of 10.5 mK in a dilution refrigerator located deep underground in the Gran Sasso National Laboratories, represents the largest thermal detector ever operated. The detector exhibited an energy resolution spanning a range from 3.9 keV (at 145 keV) to 7.8 keV (at the 2615 gamma-line of 208Tl) FWHM. We discuss the decrease in the background per unit mass that can be achieved increasing the mass of a bolometer.

L. Cardani; L. Gironi; J. W. Beeman; I. Dafinei; Z. Ge; G. Pessina; S. Pirro; Y. Zhu

2011-06-03T23:59:59.000Z

53

Spectroscopy of Solar Neutrinos  

E-Print Network (OSTI)

In the last years, liquid-scintillator detectors have opened a new window for the observation of low-energetic astrophysical neutrino sources. In 2007, the solar neutrino experiment Borexino began its data-taking in the Gran Sasso underground laboratory. High energy resolution and excellent radioactive background conditions in the detector allow the first-time spectroscopic measurement of solar neutrinos in the sub-MeV energy regime. The experimental results of the Beryllium-7 neutrino flux measurements as well as the prospects for the detection of solar Boron-8, pep and CNO neutrinos are presented in the context of the currently discussed ambiguities in solar metallicity. In addition, the potential of the future SNO+ and LENA experiments for high-precision solar neutrino spectroscopy will be outlined.

Michael Wurm; Franz von Feilitzsch; Marianne Goeger-Neff; Tobias Lachenmaier; Timo Lewke; Quirin Meindl; Randoplh Moellenberg; Lothar Oberauer; Walter Potzel; Marc Tippmann; Christoph Traunsteiner; Juergen Winter

2010-04-06T23:59:59.000Z

54

Nuclear Processes at Solar Energy  

E-Print Network (OSTI)

LUNA, Laboratory for Underground Nuclear Astrophysics at Gran Sasso, is measuring fusion cross sections down to the energy of the nucleosynthesis inside stars. Outstanding results obtained up to now are the cross-section measurements within the Gamow peak of the Sun of $^{3}He(^{3}He,2p)^{4}He$ and the $D(p,\\gamma)^{3}He$. The former plays a big role in the proton-proton chain, largely affecting the calculated solar neutrino luminosity, whereas the latter is the reaction that rules the proto-star life during the pre-main sequence phase. The implications of such measurements will be discussed. Preliminary results obtained last year on the study of $^{14}N(p,\\gamma)^{15}O$, the slowest reaction of the CNO cycle, will also be shown.

Carlo Broggini

2003-08-29T23:59:59.000Z

55

Neutrino astronomy with the MACRO detector  

E-Print Network (OSTI)

High energy gamma ray astronomy is now a well established field and several sources have been discovered in the region from a few GeV up to several TeV. If sources involving hadronic processes exist, the production of photons would be accompanied by neutrinos too. Other possible neutrino sources could be related to the annihilation of WIMPs at the center of galaxies with black holes. We present the results of a search for point-like sources using 1100 upward-going muons produced by neutrino interactions in the rock below and inside the MACRO detector in the underground Gran Sasso Laboratory. These data show no evidence for a possible neutrino point-like source or for possible correlations between gamma ray bursts and neutrinos. They have been used to set flux upper limits for candidate point-like sources which are in the range 10^-14-10^-15 cm-2 s-1.

M. Ambrosio

2000-02-26T23:59:59.000Z

56

The Observation of Up-going Charged Particles Produced by High Energy Muons in Underground Detectors  

E-Print Network (OSTI)

An experimental study of the production of up-going charged particles in inelastic interactions of down-going underground muons is reported, using data obtained from the MACRO detector at the Gran Sasso Laboratory. In a sample of 12.2 10^6 single muons, corresponding to a detector livetime of 1.55 y, 243 events are observed having an up-going particle associated with a down-going muon. These events are analysed to determine the range and emission angle distributions of the up-going particle, corrected for detection and reconstruction efficiency. Measurements of the muon neutrino flux by underground detectors are often based on the observation of through-going and stopping muons produced in $\

The MACRO Collaboration; M. Ambrosio et al

1998-07-31T23:59:59.000Z

57

TTRDC - Publications - TransForum Volume 11 Number 1  

NLE Websites -- All DOE Office Websites (Extended Search)

Simulator Makes Green Racing Real Simulator Makes Green Racing Real green racing sim trailer Artist's mockup of future Green Racing Simulator Trailer. Larger image. Ever want to drive a race car? Now you can, with Argonne's Green Racing Simulator. Working with the American LeMans Series (ALMS), and developed by transportation researchers Danny Bocci and Forrest Jehlik, the simulator allows a person to have a racetrack experience with a difference-the simulated race car uses green transportation technologies. How the Simulator Works Sit in the seat and start the engine! The racing simulator uses a gaming system and a computer to display Green Racing in action. The simulator, created by Danny Bocci, is based upon the recently released game Gran Tourismo 5 for the Playstation 3, with additional computers wrapping around

58

JOHN DAVIS: Ahora vayamos con Yolanda Vázquez y las más recientes motor news  

NLE Websites -- All DOE Office Websites (Extended Search)

Ahora vayamos con Yolanda Vázquez y las más recientes motor news. Ahora vayamos con Yolanda Vázquez y las más recientes motor news. YOLANDA VAZQUEZ: A pesar de las positivas noticias sobre combustibles alternativos y autos eléctricos, la mayoría de los consumidores están adoptando una actitud de esperar para ver. Pero cuando se trata de flotas públicas y comerciales, los cambios van a toda velocidad. YOLANDA VAZQUEZ: Aunque la velocidad no es el tema, es significativo que la Indianapolis Motor Speedway haya sido seleccionada para la Cumbre de Ciudades Limpias del Departamento de Energía de Estados Unidos. Gran parte de la tecnología automotriz actual surgió de la mítica carrera de Indianapolis 500. YOLANDA VAZQUEZ: A medida que una procesión de autos de combustibles alternativos se paseaba por la pista de dos millas y media, se hizo evidente que lo

59

¿A dónde se va la energía?  

NLE Websites -- All DOE Office Websites (Extended Search)

¿A dónde se va la energía? ¿A dónde se va la energía? Sólo aproximadamente el 14% -26% de la energía del combustible que usted pone en su tanque se usa para mover su coche o operar accesorios útiles, como el aire acondicionado. El resto de la energía es perdida en ineficiencias del motor, de la líínea de conducción y al estar a ralentí. Por lo tanto, el potencial para mejorar la eficiencia del combustible con tecnologías avanzadas es enorme. Combinadas Ciudad Carretera Conducir en Ciudad Los requerimientos de energía mostrados en el diagrama se calcularon conduciendo por la ciudad en el modo para-avanzar usando el procedimiento de la EPA FTP-75 Test. Perdidas de Motor En vehículos propulsados por gasolina, gran parte de la energía del combustible se pierde en el motor, primordialmente al calentarse. Pequeñas

60

FISICA: The Florida Image Slicer for Infrared Cosmology & Astrophysics  

E-Print Network (OSTI)

We report on the design, fabrication, and on-sky performance of the Florida Image Slicer for Infrared Cosmology and Astrophysics (FISICA)- a fully-cryogenic all-reflective image-slicing integral field unit for the FLAMINGOS near-infrared spectrograph. Designed to accept input beams near f/15, FISICA with FLAMINGOS provides R \\sim 1300 spectra over a 16x33-arcsec field-of-view on the Cassegrain f/15 focus of the KPNO 4-meter telescope, or a 6x12-arcsec field-of-view on the Nasmyth or Bent Cassegrain foci of the Gran Telescopio Canarias 10.4-meter telescope. FISICA accomplishes this using three sets of "monolithic" powered mirror arrays, each with 22 mirrored surfaces cut into a single piece of aluminum. We review the optical and opto-mechanical design and fabrication of FISICA, as well as laboratory test results for FISICA integrated with the FLAMINGOS instrument. Finally, we present performance results from observations with FISICA at the KPNO 4-m telescope and comparisons of FISICA performance to other available IFUs on 4-m to 8-m-class telescopes.

Stephen Eikenberry; S. Nicholas Raines; Nicolas Gruel; Richard Elston; Rafael Guzman; Jeff Julian; Glenn Boreman; Paul Glenn; Greg Hull-Allen; Jeff Hoffmann; Michael Rodgers; Kevin Thompson; Scott Flint; Lovell Comstock; Bruce Myrick

2006-04-27T23:59:59.000Z

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61

Spontaneous Muon Emission during Fission, a New Nuclear Radioactivity  

E-Print Network (OSTI)

In this paper the essential theoretical predictions for the nuclear muonic radioactivity are presented by using a special fission-like model similar with that used in description of the pionic emission during fission. Hence, a fission-like model for the muonic radioactivity takes into account the essential degree of freedom of the system: muon-fissility, muon-fission barrier height, etc. Using this model it was shown that most of the SHE-nuclei lie in the region where the muonic fissility parameters attain their limiting value X=1. Hence, the SHE-region is characterized by the absence of a classical barrier toward spontaneous muon and pion emissions. Numerical estimations on the yields for the natural muonic radioactivities of the transuranium elements as well numerical values for barrier heights are given only for even-even parent nuclei. Some experimental results from LCP-identification emission spectrum are reviewed. Also, the experimental results obtained by Khryachkov et al, using new spectrometer for investigation of ternary nuclear fission, are presented. The OPERA-experiment proposed to perform search for muonic radioactivity from lead nuclei, in the low background conditions offered by the Gran Sasso underground Laboratory (LNGS), is discussed.

D. B. Ion; M. L. D. Ion; Reveica Ion-Mihai

2011-01-24T23:59:59.000Z

62

Results from a search for the 0 {nu}{beta}{beta}-decay of {sup 130}Te  

SciTech Connect

A detailed description of the CUORICINO {sup 130}Te neutrinoless double-beta (0 {nu}{beta}{beta}) decay experiment is given and recent results are reported. CUORICINO is an array of 62 tellurium oxide (TeO{sub 2}) bolometers with an active mass of 40.7 kg. It is cooled to {approx}8-10 mK by a dilution refrigerator shielded from environmental radioactivity and energetic neutrons. It is running in the Laboratori Nazionali del Gran Sasso (LNGS) in Assergi, Italy. These data represent an exposure of 11.83 kg yr or 91 mole-years of {sup 130}Te. No evidence for 0 {nu}{beta}{beta}-decay was observed and a limit of T{sub 1/2}{sup 0} {sup {nu}}({sup 130}Te){>=}3.0x10{sup 24} y (90% CL) is set. This corresponds to an upper limit on the effective mass, , between 0.19 and 0.68 eV when analyzed with the many published nuclear structure calculations. In the context of these nuclear models, the values fall within the range corresponding to the claim of evidence of 0 {nu}{beta}{beta}-decay by H. V. Klapdor-Kleingrothaus et al. The experiment continues to acquire data.

Arnaboldi, C.; Brofferio, C.; Capelli, S.; Clemenza, M.; Fiorini, E.; Nucciotti, A.; Pavan, M.; Sisti, M. [Dipartimento di Fisica dell'Universita di Milano-Bicocca, I-20126 Milano (Italy); Sezione INFN di Milano-Bicocca, I-20126 Milano (Italy); Artusa, D. R.; Avignone III, F. T.; Bandac, I.; Creswick, R. J.; Farach, H. A.; Rosenfeld, C. [Department of Physics and Astronomy, University of South Carolina, Columbia, SC 29208 (United States); Balata, M.; Bucci, C.; Giachero, A.; Gorla, P.; Nisi, S. [INFN Laboratori Nazionali del Gran Sasso, I-67010, Assergi (L'Aquila) (Italy); Barucci, M. [Dipartimento di Fisica dell'Universita di Firenze, I-50019 Firenze (Italy); Sezione INFN di Firenze, I-50019, Firenze (Italy)] (and others)

2008-09-15T23:59:59.000Z

63

Prompt Gamma Rays in {sup 77}Ge after Neutron Capture on {sup 76}Ge  

SciTech Connect

The observation of neutrinoless double beta decay would be proof of the Majorana nature of the neutrino. Half-lives for these decays are very long (for {sup 76}Ge:>10{sup 25} y), so background reduction and rejection is the major task for double beta experiments. The GERDA (GERmanium Detector Array) experiment at the Gran Sasso Laboratory of the INFN (LNGS) searches for neutrinoless double beta decay of {sup 76}Ge. The isotope {sup 76}Ge is an ideal candidate because it can be used as source and detector at the same time. A large remaining contribution to the background arises from the prompt gamma cascade after neutron capture by {sup 76}Ge followed by {beta}{sup -}-decay of {sup 77}Ge. Since the prompt gamma decay scheme is poorly known, measurements with isotopically enriched Germanium samples were carried out at the PGAA facility at the research reactor FRM II (Munich). With the known prompt gamma spectrum it will be possible to improve the overall veto efficiency of the GERDA experiment.

Meierhofer, Georg; Grabmayr, Peter; Jochum, Josef [Physikalisches Institut, Eberhard Karls Universitaet Tuebingen, Auf der Morgenstelle 14, 72076 Tuebingen (Germany); Canella, Lea [Institut fuer Radiochemie, Technische Universitaet Muenchen, Walther-Meissner-Str. 3, 85748 Garching (Germany); Jolie, Jan; Kudejova, Petra; Warr, Nigel [Institut fuer Kernphysik, Universitaet zu Koeln, Zuelpicher Str. 77, 50937 Cologne (Germany)

2009-01-28T23:59:59.000Z

64

TITLE  

Office of Legacy Management (LM)

-. -. i . , . United States Government L-u+-tw / S / V ~ f Department of nersy memorandum D i T E June 0 5 , 1995 FEP-Y ATTK OF: EM-421 (U. A. Williams, 301-903-8149) SUGJECT Hazard Assessmnt f o r Radioactive Contamination a t the Associate. A i r c r a f t Site, F a i r f i e l d , Ohio To L. Price, OR This memorandum i s t o ' provide comments and approval o f the Associate i r ft i t n f o r e n ' i A r c a S eHazardAssessmet I d t i f e d S o i l C ~ m i n a t i o n . The hazard assessment was prepared and supplemental 1 i m i t s were requested, based on a single s o i l sample w i t h 134 picocuries per gran o f uranium. This sample was obtained from underneath the b u i l d i n g slab i n an area t h a t was a loading dock f o r the f a c i l i t y during Atomic Energy Comnission operations during the 1950s. The area i s n o t r e

65

¿Cómo funcionan los Híbridos?  

NLE Websites -- All DOE Office Websites (Extended Search)

¿Cómo funcionan los Híbridos? ¿Cómo funcionan los Híbridos? Diagrama de los componentes de un híbrido completo, incluyen (1) un motor de combustión interna (2) un motor eléctrico, (3) un generador, (4) una aparato de cambio de motor, and (5) una batería de gran capacidad. en inglés Flash Animation: ¿Cómo funcionan los Híbridos? (Requiere versión Flash 6.0 o superior) HTML Version: ¿Cómo funcionan los Híbridos? Los vehículos Híbridos-eléctricos (VHEs) combinan las ventajas de los motores de gasolina con los motores eléctricos y se pueden configurar para diferentes objetivos, como mejorar el ahorro de combustible, aumentar su fuerza, o proveer fuerza adicional para el uso del sistema eléctrico o los componentes electrónicos. Algunas de las tecnologías avanzadas que usan los híbridos típicamente

66

Centro de Energías Renovables (CER) en español | Open Energy Information  

Open Energy Info (EERE)

en español en español Jump to: navigation, search CER.png El CER es una institución que consolida los esfuerzos del Gobierno de Chile para desarrollar las energías renovables no convencionales (ERNC) y será un núcleo central de información y apoyo a la promoción de inversiones y transferencia tecnológica en esta materia. Este nuevo organismo es resultado del trabajo conjunto de la Comisión Nacional de Energía (CNE) y CORFO. La misión La misión del CER es promover y facilitar el desarrollo de la industria de las ERNC, articulando esfuerzos públicos y privados que optimicen el uso del gran potencial de recursos energéticos renovables no convencionales existentes en Chile, contribuyendo así a lograr un abastecimiento de energía seguro y sustentable económica, ambiental y socialmente.

67

Determinacion de la Irradiancion Solar Sobre el Territorio de Cuba a Partir  

Open Energy Info (EERE)

Determinacion de la Irradiancion Solar Sobre el Territorio de Cuba a Partir Determinacion de la Irradiancion Solar Sobre el Territorio de Cuba a Partir de Imágenes de Satelites Dataset Summary Description (Abstract): 31Conclusiones y recomendacionesEl método de cálculo de la radiación solar global desarrollado ha obtenido resultadoscomparables a otros métodos revisados en la bibliografía. A diferencia de muchos deestos métodos, que han sido ajustados y refinados por sus autores a lo largo de variosaños de trabajo, este es completamente nuevo y parte de un enfoque diferente, por loque tiene un gran potencial de ajuste y sintonización.Algunos cambios que pueden sugerirse son tomar distribuciones espaciales ytemporales del albedo, del índice de aerosoles y el contenido total de ozono y no valoresmedios constantes , lo que mejoraría el desempeño del modelo

68

The low-temperature energy calibration system for the CUORE bolometer array  

E-Print Network (OSTI)

The CUORE experiment will search for neutrinoless double beta decay (0nDBD) of 130Te using an array of 988 TeO_2 bolometers operated at 10 mK in the Laboratori Nazionali del Gran Sasso (Italy). The detector is housed in a large cryogen-free cryostat cooled by pulse tubes and a high-power dilution refrigerator. The TeO_2 bolometers measure the event energies, and a precise and reliable energy calibration is critical for the successful identification of candidate 0nDBD and background events. The detector calibration system under development is based on the insertion of 12 gamma-sources that are able to move under their own weight through a set of guide tubes that route them from deployment boxes on the 300K flange down into position in the detector region inside the cryostat. The CUORE experiment poses stringent requirements on the maximum heat load on the cryostat, material radiopurity, contamination risk and the ability to fully retract the sources during normal data taking. Together with the integration into a unique cryostat, this requires careful design and unconventional solutions. We present the design, challenges, and expected performance of this low-temperature energy calibration system.

S. Sangiorgio; L. M. Ejzak; K. M. Heeger; R. H. Maruyama; A. Nucciotti; M. Olcese; T. S. Wise; A. L. Woodcraft

2009-08-03T23:59:59.000Z

69

Commissioning Run of the CRESST-II Dark Matter Search  

E-Print Network (OSTI)

The CRESST cryogenic direct dark matter search at Gran Sasso, searching for WIMPs via nuclear recoil, has been upgraded to CRESST-II by several changes and improvements.We present the results of a commissioning run carried out in 2007. The basic element of CRESST-II is a detector module consisting of a large (~ 300 g) CaWO_4 crystal and a very sensitive smaller (~ 2 g) light detector to detect the scintillation light from the CaWO_4.Information from light-quenching factor studies allows the definition of a region of the energy-light yield plane which corresponds to tungsten recoils. A neutron test is reported which supports the principle of using the light yield to identify the recoiling nucleus. Data obtained with two detector modules for a total exposure of 48 kg-days are presented. Judging by the rate of events in the "all nuclear recoils" acceptance region the apparatus shows a factor ~ten improvement with respect to previous results, which we attribute principally to the presence of the neutron shield. In the "tungsten recoils" acceptance region three events are found, corresponding to a rate of 0.063 per kg-day. Standard assumptions on the dark matter flux, coherent or spin independent interactions,then yield a limit for WIMP-nucleon scattering of 4.8 \\times 10^{-7}pb, at M{WIMP} ~50 GeV.

G. Angloher; M. Bauer; I. Bavykina; A. Bento; A. Brown; C. Bucci; C. Ciemniak; C. Coppi; G. Deuter; F. von Feilitzsch; D. Hauff; S. Henry; P. Huff; J. Imber; S. Ingleby; C. Isaila; J. Jochum; M. Kiefer; M. Kimmerle; H. Kraus; J. -C. Lanfranchi; R. F. Lang; B. Majorovits; M. Malek; R. McGowan; V. B. Mikhailik; E. Pantic; F. Petricca; S. Pfister; W. Potzel; F. Proebst; W. Rau; S. Roth; K. Rottler; C. Sailer; K. Schaeffner; J. Schmaler; S. Scholl; W. Seidel; L. Stodolsky; A. J. B. Tolhurst; I. Usherov; W. Westphal

2008-09-10T23:59:59.000Z

70

Sensitivity of CUORE to Neutrinoless Double-Beta Decay  

SciTech Connect

In this paper, we study the sensitivity of CUORE, a bolometric double-beta decay experiment under construction at the Laboratori Nazionali del Gran Sasso in Italy. Two approaches to the computation of experimental sensitivity are discussed and compared, and the formulas and parameters used in the sensitivity estimates are provided. Assuming a background rate of 10{sup -2} cts/(keV kg y), we find that, after 5 years of live time, CUORE will have a 1#27;{sigma} sensitivity to the neutrinoless double-beta decay half-life of {caret T{sup 0{nu}}{sub 1/2}}(1{sigma}#27;) = 1.6x#2;10{sup 26} y and thus a potential to probe the effective Majorana neutrino mass down to 41-95 meV; the sensitivity at 1.64{sigma}#27;, which corresponds to 90% C.L., will be {caret T{sup 0{nu}}{sub 1/2}(1.64{sigma}#27;}) = 9.5x10{sup 25} y. This range is compared with the claim of observation of neutrinoless double-beta decay in {sup 76}Ge and the preferred range in the neutrino mass parameter space from oscillation results.

CUORE; Alessandria, F.; Andreotti, E.; Ardito, R.; Arnaboldi, C.; Avignone III, F. T.; Balata, M.; Bandac, I.; Banks, T. I.; Bari, G.; Beeman, J.; Bellini, F.; Bersani, A.; Biassoni, M.; Bloxham, T.; Brofferio, C.; Bryant, A.; Bucci, C.; Cai, X. Z.; Canonica, L.; Capelli, S.; Carbone, L.; Cardani, L.; Carrettoni, M.; Casali, N.; Chott, N.; Clemenza, M.; Cosmelli, C.; Cremonesi, O.; Creswick, R. J.; Dafinei, I.; Dally, A.; Biasi, A. De; Decowski, M. P.; Deninno, M. M.; Waard, A. de; Domizio, S. Di; Ejzak, L.; Faccini, R.; Fang, D. Q.; Farach, H. A.; Ferri, E.; Ferroni, F.; Fiorini, E.; Foggetta, L.; Franceschi, M. A.; Freedman, S. J.; Frossati, G.; Fujikawa, B. K.; Giachero, A.; Gironi, L.; Giuliani, A.; Gorla, P.; Gotti, C.; Guardincerri, E.; Gutierrez, T. D.; Haller, E. E.; Han, K.; Heeger, K. M.; Huang, H. Z.; Ichimura, K.; Kadel, R.; Kazkaz, K.; Keppel, G.; Kogler, L.; Kolomensky, Yu. G.; Kraft, S.; Lenz, D.; Li, Y. L.; Liu, X.; Longo, E.; Ma, Y. G.; Maiano, C.; Maier, G.; Maino, M.; Mancini, C.; Martinez, C.; Martinez, M.; Maruyama, R. H.; Moggi, N.; Morganti, S.; Napolitano, T.; Newman, S.; Nisi, S.; Nones, C.; Norman, E. B.; Nucciotti, A.; Orio, F.; Orlandi, D.; Ouellet, J. L.; Pallavicini, M.; Palmieri, V.; Pattavina, L.; Pavan, M.; Pedretti, M.; Pessina, G.; Pirro, S.; Previtali, E.; Rampazzo, V.; Rimondi, F.; Rosenfeld, C.; Rusconi, C.; Salvioni, C.; Sangiorgio, S.; Schaeffer, D.; Scielzo, N. D.; Sisti, M.; Smith, A. R.; Stivanello, F.; Taffarello, L.; Terenziani, G.; Tian, W. D.; Tomei, C.; Trentalange, S.; Ventura, G.; Vignati, M.; Wang, B. S.; Wang, H. W.; Whitten Jr., C. A.; Wise, T.; Woodcraft, A.; Xu, N.; Zanotti, L.; Zarra, C.; Zhu, B. X.; Zucchelli, S.

2011-11-23T23:59:59.000Z

71

Why is the Conclusion of the GERDA Experiment Wrong ?  

E-Print Network (OSTI)

The first results of the GERDA double beta experiment in Gran Sasso were recently presented. They are fully consistent with the Heidelberg-Moscow experiment, but because of its low statistics cannot proof anything at this moment. It is no surprise that the statistics is still far from being able to test the signal claimed by the Heidelberg-Moscow (HM) experiment. The energy resolution of the coaxial detectors is a factor of 1.5 worse than in the HM experiment. The original goal of background reduction to 10^{-2}counts/kgykeV, or by an order of magnitude compared to the Heidelberg-Moscow experiment, has not been reached. The background is only a factor 2.3 lower if we refer it to the experimental line width, i.e. in units counts/kgy energy resolution. With pulse shape analysis (PSA) the background in the HM experiment around Q_{\\beta\\beta} is 4x10^{-3} counts/kgykeV \\cite{HVKK-IVK-MPhLA2006}, which is a factor of 4 (5 referring to the line width) lower than that of GERDA with pulse shape analysis. The amount o...

Klapdor-Kleingrothaus, Hans Volker; Karpov, Sergey N

2013-01-01T23:59:59.000Z

72

Discriminating among Earth composition models using geo-antineutrinos  

E-Print Network (OSTI)

It has been estimated that the entire Earth generates heat corresponding to about 40 TW (equivalent to 10,000 nuclear power plants) which is considered to originate mainly from the radioactive decay of elements like U, Th and K, deposited in the crust and mantle of the Earth. Radioactivity of these elements produce not only heat but also antineutrinos (called geo-antineutrinos) which can be observed by terrestrial detectors. We investigate the possibility of discriminating among Earth composition models predicting different total radiogenic heat generation, by observing such geo-antineutrinos at Kamioka and Gran Sasso, assuming KamLAND and Borexino (type) detectors, respectively, at these places. By simulating the future geo-antineutrino data as well as reactor antineutrino background contributions, we try to establish to which extent we can discriminate among Earth composition models for given exposures (in units of kt$\\cdot$ yr) at these two sites on our planet. We use also information on neutrino mixing pa...

Nunokawa, H; Zukanovich-Funchal, R

2003-01-01T23:59:59.000Z

73

Radiochemical Solar Neutrino Experiments - Successful and Otherwise.  

SciTech Connect

Over the years, several different radiochemical systems have been proposed as solar neutrino detectors. Of these, two achieved operating status and obtained important results that helped to define the current field of neutrino physics: the first solar-neutrino experiment, the Chlorine Detector ({sup 37}Cl) that was developed by chemist Raymond Davis and colleagues at the Homestake Mine, and the subsequent Gallium ({sup 71}Ga) Detectors that were operated by (a) the SAGE collaboration at the Baksan Laboratory and (b) the GALLEX/GNO collaborations at the Gran Sasso National Laboratory. These experiments have been extensively discussed in the literature and in many previous International Neutrino Conferences. In this paper, I present important updates to the results from SAGE and GALLEX/GNO. I also review the principles of the radiochemical detectors and briefly describe several different detectors that have been proposed. In light of the well-known successes that have been subsequently obtained by real-time neutrino detectors such as Kamiokande, Super-Kamiokande, SNO, and KamLAND, I do not anticipate that any new radiochemical neutrino detectors will be built. At present, only SAGE is still operating; the Chlorine and GNO radiochemical detectors have been decommissioned and dismantled.

Hahn,R.L.

2008-05-25T23:59:59.000Z

74

Measurement of the solar 8B neutrino rate with a liquid scintillator target and 3 MeV energy threshold in the Borexino detector  

E-Print Network (OSTI)

We report the measurement of electron neutrino elastic scattering from 8B solar neutrinos with 3 MeV energy threshold by the Borexino detector in Gran Sasso (Italy). The rate of solar neutrino-induced electron scattering events above this energy in Borexino is 0.217 +- 0.038 (stat) +- 0.008 (syst) cpd/100 t, which corresponds to the equivalent unoscillated flux of (2.4 +- 0.4 (stat) +- 0.1 (syst))x10^6 cm^-2 s^-1, in good agreement with measurements from SNO and SuperKamiokaNDE. Assuming the 8B neutrino flux predicted by the high metallicity Standard Solar Model, the average 8B neutrino survival probability above 3 MeV is measured to be 0.29+-0.10. The survival probabilities for 7Be and 8B neutrinos as measured by Borexino differ by 1.9 sigma. These results are consistent with the prediction of the MSW-LMA solution of a transition in the solar electron neutrino survival probability between the low energy vacuum-driven and the high-energy matter-enhanced solar neutrino oscillation regimes.

The Borexino Collaboration

2008-08-21T23:59:59.000Z

75

A measurement of the 2 neutrino double beta decay rate of Te-130 in the CUORICINO experiment  

Science Conference Proceedings (OSTI)

CUORICINO was a cryogenic bolometer experiment designed to search for neutrinoless double beta decay and other rare processes, including double beta decay with two neutrinos (2{nu}{beta}{beta}). The experiment was located at Laboratori Nazionali del Gran Sasso and ran for a period of about 5 years, from 2003 to 2008. The detector consisted of an array of 62 TeO{sub 2} crystals arranged in a tower and operated at a temperature of #24;10 mK. Events depositing energy in the detectors, such as radioactive decays or impinging particles, produced thermal pulses in the crystals which were read out using sensitive thermistors. The experiment included 4 enriched crystals, 2 enriched with {sup 130}Te and 2 with {sup 128}Te, in order to aid in the measurement of the 2{nu}{beta}{beta} rate. The enriched crystals contained a total of #24;350 g {sup 130}Te. The 128-enriched (130-depleted) crystals were used as background monitors, so that the shared backgrounds could be subtracted from the energy spectrum of the 130- enriched crystals. Residual backgrounds in the subtracted spectrum were fit using spectra generated by Monte-Carlo simulations of natural radioactive contaminants located in and on the crystals. The 2{nu}{beta}{beta} half-life was measured to be T{sup 2{nu}}{sub 1/2} = [9.81{+-} #6;0.96(stat){+-} 0.49(syst)]#2;x10{sup 20} y.

Kogler, Laura

2011-11-03T23:59:59.000Z

76

Observation of beta decay of In-115 to the first excited level of Sn-115  

E-Print Network (OSTI)

In the context of the LENS R&D solar neutrino project, the gamma spectrum of a sample of metallic indium was measured using a single experimental setup of 4 HP-Ge detectors located underground at the Gran Sasso National Laboratories (LNGS), Italy. A gamma line at the energy (497.48 +/- 0.21) keV was found that is not present in the background spectrum and that can be identified as a gamma quantum following the beta decay of In-115 to the first excited state of Sn-115 (9/2+ --> 3/2+). This decay channel of In-115, which is reported here for the first time, has an extremely low Q-value, Q = (2 +/- 4) keV, and has a much lower probability than the well-known ground state-ground state transition, being the branching ratio b = (1.18 +/- 0.31) 10^-6. This could be the beta decay with the lowest known Q-value. The limit on charge non-conserving beta decay of In-115 is set at 90% C.L. as tau > 4.1 10^20 y.

C. M. Cattadori; M. De Deo; M. Laubenstein; L. Pandola; V. I. Tretyak

2004-07-16T23:59:59.000Z

77

Revista Mexicana de Astronomía y Astrofísica, 38, 97–109 (2002) CHEMICAL ABUNDANCES OF NGC 5461 AND NGC 5471 DERIVED FROM ECHELLE SPECTROPHOTOMETRY  

E-Print Network (OSTI)

Presentamos espectrofotometría de alta resolución de NGC 5461 y NGC 5471, dos regiones H II gigantes en la galaxia M101. Los datos se obtuvieron con el telescopio de 2.1 m del Observatorio Astronómico Nacional en San Pedro Mártir, Baja California. Medimos las intensidades de un conjunto de líneas de recombinación de hidrógeno y de helio, así como líneas prohibidas de un gran número de iones. Calculamos las condiciones físicas en las dos nebulosas y calculamos las abundancias químicas totales tomando en cuenta las abundancias iónicas observadas así como las no observadas; estas últimas las estimamos a partir de factores de corrección de ionización (icf ’s). Para NGC 5461 los icf ’s se basan en un modelo detallado de fotoionización diseñado específicamente para este objeto (Luridiana & Peimbert 2001), mientras que para NGC 5471 se obtuvieron a partir de un modelo de fotoionización para NGC 2363 (Luridiana, Peimbert, & Leitherer 1999), región que muestra un grado de ionización muy semejante al de NGC 5471. Los icf s así determinados los comparamos con aquellos que se obtienen a partir de las fórmulas de Mathis & Rosa (1991). Dicha comparación muestra importantes discrepancias

V. Luridiana; C. Esteban; M. Peimbert; A. Peimbert

2002-01-01T23:59:59.000Z

78

Low energy solar neutrino experiments: The Soviet American Gallium Experiment (SAGE). Final report, August 12, 1988--October 31, 1994  

SciTech Connect

Two {sup 71}Ga experiments are currently in operation. The first is the 60 ton Soviet American Gallium Experiment (SAGE) at Baksan, which has recently reported a signal level of 73+18/{minus}16(stat)+5/{minus}7(syst) SNU; the second is the 30 ton GALLEX experiment at Gran Sasso, which sees 87{+-}14{+-}7 SNU. Both results are consistent, and both suggest a neutrino flux level low compared to the total expected from standard solar model calculations. It is not possible, however, to make a case for flux levels lower than the p-p prediction. Assuming the experiments are correct (Neutrino source calibrations are planned for both SAGE and GALLEX in the near future.), it is not at all clear yet whether the answer lies with the neutrino physics, solar physics, or a combination of both. Nevertheless, though solar model effects cannot be ruled out, if the Homestake and Kamiokande results are taken at face value, then these two experiments alone imply that neutrino oscillations or some similar particle physics result must be present to some degree. This report reviews the SAGE experiment and recent results. Non-radiochemical experiments are also discussed, with an emphasis on the Kamiokande water Cerenkov results.

NONE

1995-04-01T23:59:59.000Z

79

European facilities for accelerator neutrino physics: perspectives for the decade to come  

E-Print Network (OSTI)

Very soon a new generation of reactor and accelerator neutrino oscillation experiments - Double Chooz, Daya Bay, Reno and T2K - will seek for oscillation signals generated by the mixing parameter theta_13. The knowledge of this angle is a fundamental milestone to optimize further experiments aimed at detecting CP violation in the neutrino sector. Leptonic CP violation is a key phenomenon that has profound implications in particle physics and cosmology but it is clearly out of reach for the aforementioned experiments. Since late 90's, a world-wide activity is in progress to design facilities that can access CP violation in neutrino oscillation and perform high precision measurements of the lepton counterpart of the Cabibbo-Kobayashi-Maskawa matrix. In this paper the status of these studies will be summarized, focusing on the options that are best suited to exploit existing European facilities (firstly CERN and the INFN Gran Sasso Laboratories) or technologies where Europe has a world leadership. Similar considerations will be developed in more exotic scenarios - beyond the standard framework of flavor oscillation among three active neutrinos - that might appear plausible in the occurrence of anomalous results from post-MiniBooNE experiments or the CNGS.

R. Battiston; M. Mezzetto; P. Migliozzi; F. Terranova

2009-12-17T23:59:59.000Z

80

Observation of Geo-Neutrinos  

E-Print Network (OSTI)

Geo-neutrinos, electron anti-neutrinos produced in beta decays of naturally occurring radioactive isotopes in the Earth, are a unique direct probe of our planet's interior. We report the first observation at more than 3$\\sigma$ C.L. of geo-neutrinos, performed with the Borexino detector at Laboratori Nazionali del Gran Sasso. Anti-neutrinos are detected through the neutron inverse beta decay reaction. With a 252.6 ton-yr fiducial exposure after all selection cuts, we detected 9.9^{+4.1}_{-3.4}(^{+14.6}_{-8.2}) geo-neutrino events, with errors corresponding to a 68.3%(99.73%) C.L. From the $\\ln{\\cal{L}}$ profile, the statistical significance of the Borexino geo-neutrino observation corresponds to a 99.997% C.L. Our measurement of the geo-neutrinos rate is 3.9^{+1.6}_{-1.3}(^{+5.8}_{-3.2}) events/(100ton-yr). This measurement rejects the hypothesis of an active geo-reactor in the Earth's core with a power above 3 TW at 95% C.L. The observed prompt positron spectrum above 2.6 MeV is compatible with that expected from european nuclear reactors (mean base line of approximately 1000 km). Our measurement of reactor anti-neutrinos excludes the non-oscillation hypothesis at 99.60% C.L.

Borexino Collaboration

2010-03-01T23:59:59.000Z

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81

First search for double-beta decay of 184Os and 192Os  

E-Print Network (OSTI)

A search for double-beta decay of osmium has been realized for the first time with the help of an ultra-low background HPGe gamma detector at the underground Gran Sasso National Laboratories of the INFN (Italy). After 2741 h of data taking with a 173 g ultra-pure osmium sample limits on double-beta processes in 184Os have been established at the level of T_{1/2} about 10^{14}-10^{17} yr. Possible resonant double-electron captures in 184Os were searched for with a sensitivity T_{1/2} about 10^{16} yr. A half-life limit T_{1/2} > 5.3 10^{19} yr was set for the double-beta decay of 192Os to the first excited level of 192Pt. The radiopurity of the osmium sample has been investigated and radionuclides 137Cs, 185Os and 207Bi were detected in the sample, while activities of 40K, 60Co, 226Ra and 232Th were limited at the mBq/kg level.

P. Belli; R. Bernabei; F. Cappella; R. Cerulli; F. A. Danevich; S. d'Angelo; A. Di Marco; A. Incicchitti; G. P. Kovtun; N. G. Kovtun; M. Laubenstein; D. V. Poda; O. G. Polischuk; A. P. Shcherban; V. I. Tretyak

2013-01-15T23:59:59.000Z

82

Argonne TTRDC - Green Racing - Results  

NLE Websites -- All DOE Office Websites (Extended Search)

Results and Recaps Results and Recaps Green Racing Initiative - 2011 Season The Green Racing Initiative, managed by Argonne for the U.S. Department of Energy (DOE), has become an integral part of the American Le Mans Series (ALMS). The 2011 season continued the growth and acceptance of green racing activities in the Series. In August 2011, ALMS announced that it would implement Green Racing 2.0 in future races. Renewable Fuel Use The 2011 ALMS season saw the use of non-petroleum and renewable fuels become dominant. Every Green Challenge victory in the Gran Turismo (GT) category and five out of nine victories in the Le Mans Prototype (LMP) category were won by a car using advanced fuels. Underlining the significance of this movement to advanced renewable fuels is that teams and engineers from all over the world made the decision to switch to these fuels because of their performance advantages alone. There were no incentives for switching in the form of funding or extra points. ALMS goes to great lengths to balance the performance of all the cars, so the switch to these fuels was made solely because they offered better efficiency and, in some cases, more power. The Green Challenge scoring system, developed by Argonne engineers in cooperation with the ALMS, accurately reflects renewable fuels' characteristics in terms of its greenhouse gas and oil replacement attributes without rewarding their selection of these over conventional fuels. That is what makes this switch to renewable replacements for conventional oil-based fuels all the more significant.

83

OPTICAL PHOTOMETRIC GTC/OSIRIS OBSERVATIONS OF THE YOUNG MASSIVE ASSOCIATION CYGNUS OB2  

Science Conference Proceedings (OSTI)

In order to fully understand the gravitational collapse of molecular clouds, the star formation process, and the evolution of circumstellar disks, these phenomena must be studied in different Galactic environments with a range of stellar contents and positions in the Galaxy. The young massive association Cygnus OB2, in the Cygnus-X region, is a unique target to study how star formation and the evolution of circumstellar disks proceed in the presence of a large number of massive stars. We present a catalog obtained with recent optical observations in the r, i, z filters with OSIRIS, mounted on the 10.4 m Gran Telescopio CANARIAS telescope, which is the deepest optical catalog of Cyg OB2 to date. The catalog consists of 64,157 sources down to M = 0.15 M{sub Sun} at the adopted distance and age of Cyg OB2. A total of 38,300 sources have good photometry in all three bands. We combined the optical catalog with existing X-ray data of this region, in order to define the cluster locus in the optical diagrams. The cluster locus in the r - i versus i - z diagram is compatible with an extinction of the optically selected cluster members in the 2.64{sup m} < A{sub V} < 5.57{sup m} range. We derive an extinction map of the region, finding a median value of A{sub V} = 4.33{sup m} in the center of the association, decreasing toward the northwest. In the color-magnitude diagrams, the shape of the distribution of main-sequence stars is compatible with the presence of an obscuring cloud in the foreground {approx}850 {+-} 25 pc from the Sun.

Guarcello, M. G.; Wright, N. J.; Drake, J. J.; Aldcroft, T.; Kashyap, V. L. [Smithsonian Astrophysical Observatory, MS-67, 60 Garden Street, Cambridge, MA 02138 (United States); Garcia-Alvarez, D. [Instituto de Astrofisica de Canarias, E-38205 La Laguna, Tenerife (Spain); Drew, J. E. [CAR/STRI, University of Hertfordshire, College Lane, Hatfield, AL10 9AB (United Kingdom)

2012-10-15T23:59:59.000Z

84

Experimental determination of gravitomagnetic effects by means of ring lasers  

E-Print Network (OSTI)

A new experiment aimed to the detection of the gravito-magnetic Lense-Thirring effect at the surface of the Earth will be presented; the name of the experiment is GINGER. The proposed technique is based on the behavior of light beams in ring lasers, also known as gyrolasers. A three-dimensional array of ringlasers will be attached to a rigid monument; each ring will have a different orientation in space. Within the space-time of a rotating mass the propagation of light is indeed anisotropic; part of the anisotropy is purely kinematical (Sagnac effect), part is due to the interaction between the gravito-electric field of the source and the kinematical motion of the observer (de Sitter effect), finally there is a contribution from the gravito-magnetic component of the Earth (gravito-magnetic frame dragging or Lense-Thirring effect). In a ring laser a light beam traveling counterclockwise is superposed to another beam traveling in the opposite sense. The anisotropy in the propagation leads to standing waves with slightly different frequencies in the two directions; the final effect is a beat frequency proportional to the size of the instrument and its effective rotation rate in space, including the gravito-magnetic drag. Current laser techniques and the performances of the best existing ring lasers allow at the moment a sensitivity within one order of magnitude of the required accuracy for the detection of gravito-magnetic effects, so that the objective of GINGER is in the range of feasibility and aims to improve the sensitivity of a couple of orders of magnitude with respect to present. The experiment will be underground, probably in the Gran Sasso National Laboratories in Italy, and is based on an international collaboration among four Italian groups, the Technische Universitaet Muenchen and the University of Canterbury in Christchurch (NZ).

Angelo Tartaglia

2012-12-12T23:59:59.000Z

85

Uranium Lease Tracts Location Map  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

16. 16. W. R.17 W. R.18 W. R.17 W. OUTLAW MESA MAVERICK CANYON CALAMITY MESA D O LO R E S MESA COUN TY MONT ROSE COUN TY SINBAD VALLEY SAN JUAN COUN TY MONT ROSE COUN TY PARADOX P A R A D O X V A L L E Y R I V E R ATKINSON MESA URAVAN CLUB MESA BEDROCK DOLORES RIVER S A N M I G U E L R I V E R COLO RAD O UTAH R.26 W. R.19 W. R. 26 E. R. 20 W. R. 19 W. R. 18 W. SAN MIGU EL COUN TY SAN JUAN COUN TY 141 SLICK ROCK D IS A P P O IN T M E N T V A L L E Y BIG GYPSUM VALLEY DRY CREEK BASIN MONT ROSE COUN TY SAN MIGU EL COUN TY WILD STEER MESA R.17 W. DOLORES RIVER T. 25 S. T. 26 S. T. 27 S. T. 28 S. T. 29 S. T. 30 S. T. 31 S. T. 32 S. T. 48 N. T. 47 N. T. 46 N. T. 45 N. T. 44 N. T. 50 N. T. 49 N. COLO RAD O UTAH T. 43 N. 141 MONOGRAM MESA 14 1 GRAN D COUN TY R.16 W. NATURITA TO GATEWAY TO La SAL TO DOVE CREEK 141 90 NUCLA EGNAR 97 P A R A D O X V A L L E Y R.20 W. T. 51 N. 9 16 8 11 13 18 14(1) 11A 19A 19 7 20 25 21 16A 12 23(1) 6 26 10 15 13A 17(1) 24 27 22 5 22A 15A 23(3) 8A 17(2)

86

A study of the ultrahigh-energy cosmic ray mass composition with the MACRO and EAS-TOP experiments  

SciTech Connect

Two components of cosmic-ray-induced air showers are measured simultaneously at the Gran Sasso Laboratory: the electromagnetic shower at the ground surface by the EAS-TOP extensive air shower array, and the deep-underground muons by the MACRO experiment. The two independent data sets collected during 96.3 days of simultaneous running are combined, and underground muon multiplicity distributions are obtained for anticoincident events (no surface trigger) and high-energy, coincident events. These categories correspond to ranges in primary energy from about 2 x 10{sup 3} GeV to a few times 10{sup 5} GeV, and from 1.5 x 10{sup 5} GeV to about 10{sup 7} GeV, respectively. The experimental shower size and muon multiplicity distributions, as well as the distribution of mean muon multiplicity as a function of shower size (N{sub mu} - log(N{sub mu}) relation), are compared to the ones obtained with Monte Carlo calculations using various trial compositions as input. This is done in an effort to discriminate between these models of primary cosmic-ray mass composition at and above the `kneel` in the all-particle spectrum, where contradictory experimental evidence exists and where a knowledge of the composition would bear upon possible mechanisms for cosmic-ray acceleration and propagation. Detailed studies of simulated anticoincident event rates uncover problems with generator used, with between 25 and 40% too few high-energy muons created. This, combined with the dependence of absolute event rates on the assumed differential primary energy spectra, hampers the interpretation in terms of composition of underground muon or surface air shower data taken separately. However, the N{sub mu} - log(N{sub e}) relation is independent of the spectra or overall Monte Carlo normalization problems. The simulated N{sub mu} - log (N{sub e}) relation for coincident events is found to be inconsistent with the possibility that the cosmic ray flux becomes proton-dominated at and above the knee.

Coutu, S.

1993-12-31T23:59:59.000Z

87

Neutron Interactions in the CUORE Neutrinoless Double Beta Decay Experiment  

SciTech Connect

Neutrinoless double beta decay (0{nu}DBD) is a lepton-number violating process that can occur only for a massive Majorana neutrino. The search for 0{nu}DBD is currently the only practical experimental way to determine whether neutrinos are identical to their own antiparticles (Majorana neutrinos) or have distinct particle and anti-particle states (Dirac neutrinos). In addition, the observation of 0{nu}DBD can provide information about the absolute mass scale of the neutrino. The Cuoricino experiment was a sensitive search for 0{nu}DBD, as well as a proof of principle for the next generation experiment, CUORE. CUORE will search for 0{nu}DBD of {sup 130}Te with a ton-scale array of unenriched TeO{sub 2} bolometers. By increasing mass and decreasing the background for 0{nu}DBD, the half-life sensitivity of CUORE will be a factor of twenty better than that of Cuoricino. The site for both of these experiments is the Laboratori Nazionali del Gran Sasso, an underground laboratory with 3300 meters water equivalent rock overburden and a cosmic ray muon attenuation factor of 10{sup -6}. Because of the extreme low background requirements for CUORE, it is important that all potential sources of background in the 0{nu}DBD peak region at 2530 keV are well understood. One potential source of background for CUORE comes from neutrons, which can be produced underground both by ({alpha},n) reactions and by fast cosmic ray muon interactions. Preliminary simulations by the CUORE collaboration indicate that these backgrounds will be negligible for CUORE. However, in order to accurately simulate the expected neutron background, it is important to understand the cross sections for neutron interactions with detector materials. In order to help refine these simulations, I have measured the gamma-ray production cross sections for interactions of neutrons on the abundant stable isotopes of Te using the GEANIE detector array at the Los Alamos Neutron Science Center. In addition, I have used the GEANIE data to set an upper limit for the production of a 2529 keV gamma-ray from the {sup 126}Te(n,n{prime}{gamma}) reaction. This gamma-ray is a potential source of interference for the 0{nu}DBD peak. Based on this measurement, the contribution of this line to the background is expected to be negligible.

Dolinski, M J

2008-09-24T23:59:59.000Z