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

被引:971
作者
Douchin, F
Haensel, P
机构
[1] Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland
[2] Univ Illinois, Dept Phys, Urbana, IL 61801 USA
[3] Ecole Normale Super Lyon, Ctr Rech Astron Lyon, F-69364 Lyon, France
关键词
dense matter; equation of state; stars : neutron;
D O I
10.1051/0004-6361:20011402
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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(circle dot) and 2.05 M(circle dot), respectively. Effects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.
引用
收藏
页码:151 / 167
页数:17
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