Abstract

This web site provides equation of state (EOS) for neutron star matter. The chiral quark-meson coupling (CQMC) model within relativistic Hartree-Fock approximation is adopted for uniform nuclear matter. All octet baryons are considered in the core region, while only Ξ^- appears in neutron stars. In the crust region, nuclei are taken into account within the Thomas-Fermi calculation. For the details, see Miyatsu et al. (2013), arXiv:1308.6121 [astro-ph.HE]. This EOS table is open for general use in any numerical simulations for astrophysics, provided that our paper is referenced in your publication.

User's Guide (read me first)

• guide.pdf (55.7kB)

EOS tables

• Baryon mass density, energy density, pressure and lepton (= electron + muon) fraction (26.8kB)
• Particle fractions (68.8kB)
• Properties of nuclei in the crust region (13.1kB)

Key parameters

• Saturation density: 0.155 fm^-3
• Saturation energy: -16.1 MeV
• Symmetry energy: 33.6 MeV (32.7 MeV)
• Slope of symmetry energy: 77.1 MeV (75.8 MeV)
• Incompressibility: 274 MeV
• Maximum mass of neutron star: 1.95M_solar

Note: There are two diffinitions of symmetry energy. See Section 3.2 and Table 2 of our paper for the details.

Contact

• Tsuyoshi Miyatsu
• Department of Physics, Soongsil University
• Seoul 156-743, Korea
• E-mail: tmiyatsu@ssu.ac.kr

• Ken'ichiro Nakazato
• Department of Physics, Faculty of Science & Technology, Tokyo University of Science
• 2641 Yamazaki, Noda, Chiba 278-8510, Japan
• E-mail: nakazato@rs.tus.ac.jp

Reference

Please reference the following paper when you publish scientific articles using this EOS.

• A new equation of state for neutron star matter with nuclei in the crust and hyperons in the core,
  T. Miyatsu, S. Yamamuro, and K. Nakazato,
  arXiv:1308.6121 [astro-ph.HE]