Constraints on and consequences of a 17-keV neutrino

Details Constraints on and consequences of a 17-keV neutrino Constraints on and consequences of a 17-keV neutrino

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992nuphs..28..148c&link_type=abstract

Nuclear Physics B Proceedings Supplements, Volume 28, Issue 1, p. 148-152.

Physics

Nuclear Physics

Scientific paper

If the 17-keV neutrino exists, various constraints require that (1) it be a Majorana neutrino which is mainly ντ (2) it not be the dark matter of the universe, although its existence would rule out dominant hot dark matter; (3) the νμ be a heavy Majorana neutrino of mass 17 keV or in the range 190-270 keV; and (4) the MSW solution to the solar neutrino problem involve νe conversion to a light sterile neutrino. Crucial to these conclusions is ruling out a 17-keV Dirac neutrino because it would have cooled supernova 1987A too rapidly for the duration of the neutrino pulses observed by Kamiokande and IMB. Reasons for strengthening that argument are given, and possible loopholes for avoiding it are explored. The resulting possibilities for neutrino masses point to follow-on experiments, which are discussed.

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