Neutron Stars in a Chiral Model with Finite Temperature
V. Dexheimer, S. Schramm, H. Stoecker
TL;DR
This paper models neutron star matter using a chiral approach with finite temperature, analyzing effects of baryonic resonances, neutrino trapping, and entropy on neutron star properties like mass and radius.
Contribution
It introduces a hadronic chiral model with SU(3) multiplets to study neutron stars at finite temperature, including proto-neutron star conditions.
Findings
Consistent nuclear matter and finite nuclei results.
Neutron star mass and radius predictions.
Effects of baryonic resonances and temperature on star properties.
Abstract
Neutron star matter is investigated in a hadronic chiral model approach using the lowest flavor-SU(3) multiplets for baryons and mesons. The parameters are determined to yield consistent results for saturated nuclear matter as well as for finite nuclei. The influence of baryonic resonances is discussed. The global properties of a neutron star such as its mass and radius are determined. Proto-neutron star properties are studied by taking into account trapped neutrinos, temperature and entropy effects.
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.