Limits on low-energy neutrino fluxes with the Mont Blanc liquid scintillator detector

被引：31

作者：

Aglietta, M. ^{[1
]}

Antonioli, P. ^{[2
]}

Badino, G. ^{[2
]}

Bologna, G. ^{[2
]}

Castagnoli, C. ^{[1
,2
]}

Castellina, A. ^{[1
]}

Dadykin, V. L. ^{[3
]}

Fulgione, W. ^{[1
]}

Galeotti, P. ^{[1
,2
]}

Khalchukov, F. F. ^{[3
]}

Korolkova, E. V. ^{[3
]}

Kortchaguin, P. V. ^{[3
]}

Kortchaguin, V. B. ^{[3
]}

Kudryavtsev, V. A. ^{[3
]}

Malguin, A. S. ^{[3
]}

Periale, L. ^{[1
]}

Ryassny, V. G. ^{[3
]}

Ryazhskaya, O. G. ^{[3
]}

Saavedra, O. ^{[1
,2
]}

Trinchero, G. ^{[1
]}

Vernetto, S. ^{[1
]}

Yakushev, V. F. ^{[3
]}

Zatsepin, G. T. ^{[3
]}

机构：

[1] CNR, Ist Cosmogeofis, I-10133 Turin, Italy

[2] Univ Turin, Ist Fis Gen, I-10125 Turin, Italy

[3] Russian Acad Sci, Inst Nucl Res, Moscow 117312, Russia

来源：

ASTROPARTICLE PHYSICS | 1992年 / 1卷 / 01期

关键词：

28;

D O I：

10.1016/0927-6505(92)90004-J

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The LSD liquid scintillation detector has been operating since 1985 as an underground neutrino observatory in the Mont Blanc Laboratory with the main objective of detecting antineutrino bursts from collapsing stars. In August 1988 the construction of an additional lead and borex paraffin shield considerably reduced the radioactive background and increased the sensitivity of the apparatus. In this way the search for steady fluxes of low-energy neutrinos of different flavours through their interactions with free protons and carbon nuclei of the scintillator was made possible. No evidence for a galactic collapse was observed during the whole period of measurement. The corresponding 90% c.l. upper limit on the galactic collapses rate is 0.45 y(-1) for a burst duration of Delta T <= 10 s. After analysing the last 3 years data, the following 90% c.l. upper limits on the steady neutrino and antineutrino fluxes were obtained: Phi((nu) over bar (e)) < 9.0 x 10(4) <(nu)over bar>(e) s(-1) cm(-2), 9 <= E-nu <= 50 MeV, Phi((nu) over bar (e)) < 8.2 x 10(3) <(nu)over bar>(e) s(-1) cm(-2), 20 <= E-nu <= 50 MeV, Phi(nu(e)) < 6.8 x 10(3) nu(e) s(-1) cm(-2), 25 <= E-nu <= 50 MeV, Phi(nu(mu+tau)) < 3.0 x 107 nu(mu+tau) s(-1) cm(-2), 20 <= E-nu <= 100 MeV, Phi((nu) over bar (mu+tau)) < 3.3 x 107 <(nu)over bar>(mu+tau) s(-1) cm(-2), 20 <= E-nu <= 100 MeV. In particular comparing the obtained upper limit on the (nu) over bar (e) flux for 9 <= E-nu <= 20 MeV to the solar nu(e) flux predicted by the standard solar model in the same range of energy, we can exclude the possibility that more than 6.3% of the solar nu(e)'s flux can change to (nu) over bar (e). Finally the first limits on the flux of relic supernova neutrinos of all flavours as a function of the neutrino sea temperature are presented.

引用

页码：1 / 9

页数：9

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