Isothermal vs. isentropic description of protoneutron stars in the Brueckner-Bethe-Goldstone theory

Abstract

We study the structure of hadronic protoneutron stars within the finite temperature Brueckner-Bethe-Goldstone theoretical approach. Assuming beta-equilibrated nuclear matter with nucleons and leptons in the stellar core, with isothermal or isentropic profile, we show that particle populations and equation of state are very similar. As far as the maximum mass is concerned, we find that its value turns out to be almost independent on T, while a slight decrease is observed in the isentropic case, due to the enhanced proton fraction in the high density range.

arXiv comment12pages, 4 figures, to be published in a special issue of "Physics of Atomic Nuclei" devoted to the 85th birthday of S. Belyaev

References in corpus (5)

• An accurate nucleon-nucleon potential with charge-independence breaking
• Composition and Structure of Protoneutron Stars
• Evolution of Protoneutron Stars
• Protoneutron stars within the Brueckner-Bethe-Goldstone theory
• Limiting temperature from microscopic equation of state

Cited by in corpus (9)

• Hyperon stars at finite temperature in the Brueckner theory
• The maximum and minimum mass of protoneutron stars in the Brueckner theory
• Hybrid protoneutron stars with the Dyson-Schwinger quark model
• Oscillations of hot, young neutron stars: Gravitational wave frequencies and damping times
• Protoneutron stars in the Brueckner-Hartree-Fock approach and finite-temperature kaon condensation
• Structure of the hadron-quark mixed phase in protoneutron stars
• Study of Beta Equilibrated 2+1 Flavor Quark Matter in PNJL Model
• Nuclear matter at finite temperature and static properties of proto-neutron star
• $f$ and $p$ mode oscillation of proto-neutron stars with systematic variation of the nucleon effective mass