Volume 451, Number 1, May III 2006
|Page(s)||213 - 222|
|Section||Stellar structure and evolution|
|Published online||25 April 2006|
Protoneutron stars within the Brueckner-Bethe-Goldstone theory
Istituto Nazionale di Fisica Nucleare, Sezione di Catania, and Dipartimento di Fisica, Universitá di Catania, via S. Sofia 64, 95123 Catania, Italy e-mail: firstname.lastname@example.org
Accepted: 5 January 2006
We study the structure of newly born neutron stars (protoneutron stars) within the finite temperature Brueckner-Bethe-Goldstone theoretical approach also including hyperons. We find that for purely nucleonic stars both finite temperature and neutrino trapping reduce the value of the maximum mass. For hyperonic stars the effect is reversed, because neutrino trapping shifts the appearance of hyperons to larger baryon density and considerably stiffens the equation of state.
Key words: dense matter / equation of state / stars: interiors / stars: neutron
© ESO, 2006
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