EDP Sciences
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Volume 380, Number 1, December II 2001
Page(s) 151 - 167
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20011402

A&A 380, 151-167 (2001)
DOI: 10.1051/0004-6361:20011402

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

F. Douchin1, 2 and P. Haensel3

1  Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
2  Centre de Recherche Astronomique de Lyon, ENS de Lyon, 69364 Lyon, France
3  N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland

(Received 31 July 2001 / Accepted 10 September 2001 )

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 effective 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 first-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) npe$\mu$ 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 $0.094 M_\odot$ and $2.05 M_\odot$, respectively. Effects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.

Key words: dense matter -- equation of state -- stars: neutron

Offprint request: P. Haensel, haensel@camk.edu.pl

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