Protoneutron stars within the Brueckner-Bethe-Goldstone theory

Abstract

We study the structure of newly born neutron stars (protoneutron stars) within the finite temperature Brueckner-Bethe-Goldstone theoretical approach including also 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 stiffens considerably the equation of state.

11 pages, 7 figures, submitted to Astronomy & Astrophysics

References in corpus (2)

• Hybrid stars with the color dielectric and the MIT bag models
• Limiting temperature from microscopic equation of state

Cited by in corpus (33)

• Equations of state for supernovae and compact stars
• Quantum Monte Carlo calculation of the equation of state of neutron matter
• Hadron-quark mixed phase in hyperon stars
• Hyperon stars at finite temperature in the Brueckner theory
• Hybrid protoneutron stars with the MIT bag model
• The maximum and minimum mass of protoneutron stars in the Brueckner theory
• Hybrid equation of state approach in binary neutron-star merger simulations
• Hybrid protoneutron stars with the Dyson-Schwinger quark model
• Oscillations of hot, young neutron stars: Gravitational wave frequencies and damping times
• The Deconfinement Phase Transition in Proto-Neutron-Star Matter
• Hot neutron stars with microscopic equations of state
• Microscopic three-body forces and kaon condensation in cold neutrino-trapped matter
• Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants
• Hot hadron-quark mixed phase including hyperons
• Protoneutron stars in the Brueckner-Hartree-Fock approach and finite-temperature kaon condensation
• Equation of state for $\beta$-stable hot nuclear matter
• Binary neutron star merger simulations with hot microscopic equations of state
• Structure of the hadron-quark mixed phase in protoneutron stars
• Structure of hybrid protoneutron stars within the Nambu--Jona-Lasinio model
• Microscopic nuclear equation of state at finite temperature and stellar stability
• Hot neutron stars and their equation of state
• Nuclear matter at finite temperature and static properties of proto-neutron star
• A microscopic equation of state for protoneutron stars
• Isothermal vs. isentropic description of protoneutron stars in the Brueckner-Bethe-Goldstone theory
• Revisiting the hot matter in the center of gamma-ray bursts and supernova
• Supernovae and Weinberg's Higgs Portal Dark Radiation and Dark Matter
• Hadron-Quark Phase Transitions in Hyperon Stars
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• The property difference between the neutron star PSR J0348+0432 and its proto neutron star
• Equation of state for dense supernova matter
• Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction
• Neutrino-Neutron Scattering Opacities in Supernova Matter
• Properties of rapidly rotating hot neutron stars within Brueckner theory