EDP Sciences
Free access
Volume 366, Number 2, February I 2001
Page(s) 532 - 537
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20000090

A&A 366, 532-537 (2001)
DOI: 10.1051/0004-6361:20000090

Properties of neutron stars with hyperons in the relativistic mean field theory

Z. X. Ma1, Z. G. Dai1, 2 and T. Lu1, 2

1  Department of Astronomy, Nanjing University, Nanjing 210093, PR China
2  IHEP, Chinese Academy of Sciences, Beijing 100039, PR China

(Received 3 July 2000 / 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 $M_\odot$ is presented. Our results satisfy the requirements from observations of the mass of binary radio pulsars, and the ratio, $I_{\rm c}/I_{\rm tot}$, 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

Offprint request: T. Lu, tlu@nju.edu.cn

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