Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-17T16:13:02.542Z Has data issue: false hasContentIssue false
  • English
  • Français

Neutrinos: Detection and Interpretation

Published online by Cambridge University Press:  14 August 2015

L.N. Alexeyeva
L.N. Alexeyeva*
Affiliation:
Institute for Nuclear Research, Academy of Sciences of the USSR 60th October Anniversary Prospect 7a, 117 312 Moscow, U.S.S.R.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Observations of the neutrino burst from Supernova 1987A by water Cherenkov detectors (KAMIOKANDE II, IMB) and liquid scintillator detectors (Baksan, Mont Blanc) are reviewed. It is shown that neutrino signal from SN 1987A was observed. There are 24 events in three detectors (KAMIOKANDE II, IMB, Baksan) recorded at 7:35 UT. The average properties of the signal (effective neutrino temperature, total energy of neutrino emission, burst duration) are consistent with the general theoretical description of supernova explosions. Special attention is concentrated on individual characteristics of the signals detected and the available discrepancies of the model estimates. Time profile of the neutrino burst, estimates of effective neutrino temperatures and total neutrino energies, angular distributions of the events are discussed. These properties point out, probably, a more compound picture of the phenomenon. The more detail analysis of the experimental data is needed and all possibilities must be at least considered. Based upon the Baksan observations, an upper limit of 0.35 core collapse in the Galaxy per year (90% C.L.) is shown.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 229 - 237
Copyright
Copyright © Kluwer 1989

References

[1] Domogatsky, G. and Zatsepin, G. Proc.9th ICRC, (1965) England, London, 2, 1030.Google Scholar
[2] Bionata, R. et al. (1987) Phys.Rev.Lett. 58, 1494.Google Scholar
[2] Hiratag, K. et al. (1987) Phys.Rev.Lett. 58, 1490; (1988) Preprint UPR – 0150E, UT-ICEPP-88–03.Google Scholar
[4] Alexeyev, E. et al.(1987) JETP Lett. 45, 589; (1988) Phys. Lett. B205, 209.Google Scholar
[15] Aglietta, M. et al. (1987) Europhys.Lett. 3, 1315.Google Scholar
[6] Haxton, W. (1987) Phys.Rev. D36, 2283.Google Scholar
[7] Fukugita, M. et al. (1988) Preprint IASSNS – AST 88/25.Google Scholar
[8] Morrison, D. (1988) Preprint CERN/EP 88–9.Google Scholar
[9] Mayle, R. Wilson, J. and Schramm, D.(1987) Astroph.J. 318, 288 Google Scholar
Nadyozhin., D. (1978) Astroph.Space Sci. 53, 131;CrossRefGoogle Scholar
Araett., W. (1987) Astroph.J. 319, 136;Google Scholar
Bruenn, S. (1987) Phys.Rev. Lett. 59, 938;Google Scholar
Burrows, A.(1988) Preprint of the Steward Observatory No. 815.Google Scholar
[10] Bancall, J. et al. (1987) Preprint IASSNS-AST 87/8; Schramm, D. (1987) FERMILAB-CONF-87/161-A; Burrows, A. (1988) Preprint of Steward Observatory No 799.Google Scholar
[11] Kolb, E. et al. (1987) Phys.Rev. D35, 3598.Google Scholar
[12] Alexeyev, E. et al.(1988) Sov.Astron.Lett. 14, 41.Google Scholar
[13] Dar, A. (1988) Preprint TECHNION-PH-88–3; LoSecco.J. (1988) Preprint UND-PDK-88–4.Google Scholar
[14] Mattews, J. et al. (1987) Proc.U.of Minnesota Workshop; LoSecco.J. (1987) Preprint UND-PDK-88–3.Google Scholar
[15] Aglietta, M. et al. (1988) Report at Les Recontres de Physique de la Vallee d’Aoste, La Thuile, February 29.Google Scholar