Protoneutron stars in the Brueckner-Hartree-Fock approach and finite-temperature kaon condensation
A. Li, X. R. Zhou, G. F. Burgio, H.-J. Schulze
TL;DR
This paper investigates the properties of hot, neutrino-trapped proto-neutron stars using a combined Brueckner-Hartree-Fock nuclear matter model and a chiral model for finite-temperature kaon condensation, providing insights into their structure.
Contribution
It introduces a novel combination of Brueckner-Hartree-Fock and chiral models to study finite-temperature effects in proto-neutron stars.
Findings
Properties of hot neutrino-trapped matter characterized
Impact of kaon condensation on star stability analyzed
Equation of state refined for proto-neutron star modeling
Abstract
We study the properties of hot neutrino-trapped beta-stable stellar matter using an equation of state of nuclear matter within the Brueckner-Hartree-Fock approach including three-body forces, combined with a standard chiral model for kaon condensation at finite temperature. The properties of (proto)neutron stars are then investigated within this framework.
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