Proto-Neutron and Neutron Stars in a Chiral SU(3) Model
V. Dexheimer, S. Schramm
TL;DR
This paper uses a chiral SU(3) model to study the properties of neutron and proto-neutron stars, including phase transitions, effects of rotation, and various physical conditions.
Contribution
It introduces a comprehensive application of a hadronic chiral SU(3) model to neutron star physics, incorporating neutrino trapping, temperature, entropy, and rotation effects.
Findings
Determined star mass and radius ranges under different conditions.
Analyzed the impact of phase transitions on star stability.
Estimated maximum rotation frequencies during cooling processes.
Abstract
A hadronic chiral SU(3) model is applied to neutron and proto-neutron stars, taking into account trapped neutrinos, finite temperature and entropy. The transition to the chirally restored phase is studied and global properties of the stars like minimum and maximum masses and radii are calculated for different cases. In addition, the effects of rotation on neutron star masses are included and the conservation of baryon number and angular momentum determine the maximum frequencies of rotation during the cooling.
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