A tentative approach to the second neutrino burst of SN 1987 A

Details A tentative approach to the second neutrino burst of SN 1987 A A tentative approach to the second neutrino burst of SN 1987 A

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...191l..22h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 191, no. 2, Feb. 1988, p. L22-L24. Research supported by the Akademie der Wiss

Astronomy and Astrophysics

Astrophysics

8

Neutrinos, Supernova 1987A, Cooling, Neutron Stars, Particle Mass

Scientific paper

The mechanism responsible for the SN 1987A neutrino burst which was observed by the Baksan, Kamiokande, and IMB experiments at 07:36 UT on February 23, 1987 (4.72 h after the first burst from SN 1987A) is considered theoretically. Neutrino cooling rates for neutron stars are calculated, and it is shown that significant cooling can take place on a time scale of hours. It is proposed that the neutron star was formed at about 02:52 UT, and that its matter, having reached a critical temperature, formed a new ultradense state (pion condensate and/or quark matter) via a first-order phase transition; this transition then led to collapse of the neutron star to form an ultradense-matter star. The energy release for this transition is estimated as (1-1000) x 10 to the 50th ergs, consistent with that for the neutrino burst.

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