A microscopic equation of state for protoneutron stars

Details A microscopic equation of state for protoneutron stars A microscopic equation of state for protoneutron stars

2006-12-18

arxiv.org/abs/astro-ph/0612503v1

Astrophys.SpaceSci.308:387-394,2007

Astronomy and Astrophysics

Astrophysics

8 pages, 6 figures, to appear in Astrophysics and Space Science, Proceedings of "Isolated Neutron Stars: from the Interior to

Scientific paper

10.1007/s10509-007-9360-8

We study the structure of protoneutron stars within the finite temperature Brueckner-Bethe-Goldstone many-body theory. If nucleons, hyperons, and leptons are present in the stellar core, we find that neutrino trapping stiffens considerably the equation of state, because hyperon onsets are shifted to larger baryon density. However, the value of the critical mass turns out to be smaller than the ``canonical'' value 1.44 $M_\odot$. We find that the inclusion of a hadron-quark phase transition increases the critical mass and stabilizes it at about 1.5--1.6 $M_\odot$.

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