The phase transition from nuclear matter to quark matter during proto-neutron star evolution

Details The phase transition from nuclear matter to quark matter during proto-neutron star evolution The phase transition from nuclear matter to quark matter during proto-neutron star evolution

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.304l..25b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 304, Issue 2, pp. L25-L29.

Astronomy and Astrophysics

Astronomy

24

Equation Of State, Stars: Neutron, Supernovae: General, Supernovae: Individual: Sn 1987A

Scientific paper

We explore the occurrence of a phase transition from nuclear matter to quark matter in proto-neutron stars. To this end, we employ recent results on such a phase transition in the presence of an electron-neutrino-degenerate gas, based on a mean field model nuclear equation of state together with a quark matter equation of state as described by the MIT `bag model'. Those results show that this neutrino gas does not favour the transition. By comparison with the proto-neutron star evolutionary calculations of Keil & Janka, we find that, if the bag constant B has a value B <= 126 MeV fm^-3, the deconfinement transition indeed occurs. We also find that, if B >= 100 MeV fm^-3, the phase transition is delayed by the presence of neutrinos by a few seconds after core bounce, thus providing a natural explanation for the second peak of neutrino emission detected in SN 1987A by the Kamiokande Group. The transition to quark matter and its subsequent decay should affect proto-neutron star evolution and supernova explosions in a non-trivial way.

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