A unified equation of state of dense matter and neutron star structure

An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the eective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the application to the calculation of the properties of very neutron rich matter (Chabanat et al. 1997, 1998). The structure of the crust, and its EOS, is calculated in the T = 0 approximation, and under the assumption of the ground state composition. The crust-core transition is a very weakly rst-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) npe composition. Parameters of static neutron stars are calculated and compared with existing observational data on neutron stars. The minimum and maximum masses of static neutron stars are 0:094 M and 2:05 M, respectively. Eects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.

• Publication year

  2001

• Venue

  Astronomy and Astrophysics

• Publication date

  2001-11-05

• Fields of study

  Physics

• Identifiers
  DOI 10.1051/0004-6361:20011402arXiv astro-ph/0111092
• External record

  Open on Semantic Scholar

• Source metadata

  Semantic Scholar

• No claims are published for this paper.

• No concepts are published for this paper.

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