Search for electron antineutrino interactions with the Borexino Counting Test Facility at Gran Sasso

被引：10
|
作者：
Balata, M.
Bellini, G.
Benziger, J.
Bonetti, S.
Caccianiga, B.
Calaprice, F.
D'Angelo, D.
de Bellefon, A.
de Kerret, H.
Derbin, A.
Etenko, A.
Ford, R.
Franco, D.
Galbiati, C.
Gazzana, S.
Giammarchi, M.
Goretti, A.
Harding, E.
Heusser, G.
Ianni, A.
Ianni, A. M.
Kobychev, V. V.
Korga, G.
Kozlov, Y.
Kryn, D.
Laubenstein, M.
Lendvai, C.
Leung, M.
Litvinovich, E.
Lombardi, P.
Machulin, I.
Manuzio, D.
Manuzio, G.
Masetti, F.
Mazzucato, U.
McCarty, K.
Meroni, E.
Miramonti, L., I
Monzani, M. E.
Muratova, V.
Niedermeier, L.
Oberauer, L.
Obolensky, M.
Ortica, F.
Pallavicini, M.
Papp, L.
Perasso, L.
Pocar, A.
Raghavan, R. S.
Ranucci, G.
机构：
[1] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67010 Assergi, AQ, Italy
[2] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy
[3] Ist Nazl Fis Nucl, I-20133 Milan, Italy
[4] Princeton Univ, Dept Chem Engn, Princeton, NJ 08544 USA
[5] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[6] Tech Univ Munich, D-85747 Garching, Germany
[7] Coll France, Astroparticule & Cosmol APC, F-75231 Paris 05, France
[8] Joint Inst Nucl Res, Dubna 141980, Russia
[9] RRC Kurchatov Inst, Moscow 123182, Russia
[10] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany
[11] Kiev Inst Nucl Res, UA-06380 Kiev, Ukraine
[12] Univ Genoa, Dipartimento Fis, I-16146 Genoa, Italy
[13] Ist Nazl Fis Nucl, I-16146 Genoa, Italy
[14] Univ Perugia, Dipartimento Chim, I-06123 Perugia, Italy
[15] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA
[16] Jagiellonian Univ, M Smoluchowski Inst Phys, PL-30059 Krakow, Poland
来源：
EUROPEAN PHYSICAL JOURNAL C | 2006年 / 47卷 / 01期
基金：
美国国家科学基金会;
关键词：
D O I：
10.1140/epjc/s2006-02560-4
中图分类号：
O412 [相对论、场论]; O572.2 [粒子物理学];
学科分类号：
摘要：
Electron antineutrino interactions above the inverse beta decay energy of protons (E-(nu) over bare > 1.8 MeV) were looked for with the Borexino counting test facility (CTF). One candidate event survived after rejection of background, which included muon-induced neutrons and random coincidences. An upper limit on the solar (nu) over bar (e) flux, assumed having the B-8 solar neutrino energy spectrum, of 1.1 x 10(5) cm(-2) s(-1) (90 % C.L.) was set with a 7.8 ton x year exposure. This upper limit corresponds to a solar neutrino transition probability, nu(e) -> (nu) over bar (e) of 0.02 (90% C.L.). Predictions for antineutrino detection with Borexino, including geoneutrinos, are discussed on the basis of background measurements performed with the CTF.
引用
收藏
页码：21 / 30
页数：10
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