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Mass signature of supernova νμ and ντ neutrinos in the Sudbury Neutrino Observatory

Beacom, J. F. and Vogel, P. (1998) Mass signature of supernova νμ and ντ neutrinos in the Sudbury Neutrino Observatory. Physical Review D, 58 (9). Art. No. 093012. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:BEAprd98a

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Abstract

Core-collapse supernovae emit of order 10^58 neutrinos and antineutrinos of all flavors over several seconds, with average energies of 10–25 MeV. In the Sudbury Neutrino Observatory (SNO), which begins operation this year, neutrinos and antineutrinos of all flavors can be detected by reactions which break up the deuteron. For a future Galactic supernova at a distance of 10 kpc, several hundred events will be observed in SNO. The νμ and ντ neutrinos and antineutrinos are of particular interest, as a test of the supernova mechanism. In addition, it is possible to measure or limit their masses by their delay (determined from neutral-current events) relative to the ν̅e neutrinos (determined from charged-current events). Numerical results are presented for such a future supernova as seen in SNO. Under reasonable assumptions, and in the presence of the expected counting statistics, a νμ or ντ mass down to about 30 eV can be simply and robustly determined. If zero delay is measured, then the mass limit is independent of the distance D. At present, this seems to be the best possibility for direct determination of a νμ or ντ mass within the cosmologically interesting range. We also show how to separately study the supernova and neutrino physics, and how changes in the assumed supernova parameters would affect the mass sensitivity.


Item Type:Article
Additional Information:©1998 The American Physical Society Received 9 June 1998; published 5 October 1998 This work was supported in part by the US Department of Energy under Grant No. DE-FG03-88ER-40397. J.F.B. was supported by the Sherman Fairchild Foundation. We thank P. J. Doe, K. T. Lesko, A. B. McDonald, and E. B. Norman of the SNO Collaboration for discussions about the detector properties, and Y.-Z. Qian for discussions about supernova neutrino oscillations.
Record Number:CaltechAUTHORS:BEAprd98a
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:BEAprd98a
Alternative URL:http://dx.doi.org/10.1103/PhysRevD.58.093012
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:2542
Collection:CaltechAUTHORS
Deposited By: Archive Administrator
Deposited On:07 Apr 2006
Last Modified:26 Dec 2012 08:49

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