Proto-Neutron and Neutron Stars in a Chiral SU(3) Model

By V. Dexheimer, S. Schramm. 2008

187 citations recorded by the source corpus.

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 such as 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 determines the maximum frequencies of rotation during the cooling.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/147ff6fe3f58cfd7b834605aa0e38b20179da64e

How researchers see this paper

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In Astronomy and Astrophysics

1. J. Zdunik
2. P. Haensel
3. A. Potekhin
4. José A. Pons
5. T. Birnstiel

In Atomic and Molecular Physics, and Optics

1. J. Zdunik
2. P. Haensel

Citations in the corpus

• Antinuclei in heavy-ion collisions (2018, background): “Possible solutions include deconfinement to quark matter, or alternative Y N and Y Y couplings [212, 213, 214, 215, 216, 217, 218, 219].”
• Maximum mass of neutron stars and strange neutron-star cores (2012, background): “Dexheimer & Schramm (2008) give an earlier general discussion of vector-meson contribution to EOS.”