Volume 366, Number 2, February I 2001
|Page(s)||532 - 537|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2001|
Properties of neutron stars with hyperons in the relativistic mean field theory
Department of Astronomy, Nanjing University, Nanjing 210093, PR China
2 IHEP, Chinese Academy of Sciences, Beijing 100039, PR China
Corresponding author: T. Lu, email@example.com
Accepted: 30 October 2000
We study the equation of state (EOS) of the dense matter in the core of neutron stars with hyperons included and the star structure based on the Zimanyi & Moszkowski (ZM) model in the relativistic mean-field theory with a set of recent satisfactory parameters. The relation between hyperon abundances and baryon number densities is calculated and the distribution of baryons in the core of a typical neutron star of 1.4 is presented. Our results satisfy the requirements from observations of the mass of binary radio pulsars, and the ratio, , of the crustal momentum of inertia to the total one. The actual surface thermal radiation detected seems to indicate that baryons in the core of neutron stars should pair to form a superfluid phase, if hyperons appear in the core of neutron stars.
Key words: stars: neutron / equations of state / elementary particles
© ESO, 2001
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