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

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

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...366..532m&link_type=abstract

Astronomy and Astrophysics, v.366, p.532-537 (2001)

Astronomy and Astrophysics

Astrophysics

1

Stars: Neutron, Equations Of State, Elementary Particles

Scientific paper

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_sun is presented. Our results satisfy the requirements from observations of the mass of binary radio pulsars, and the ratio, I_c/I_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.

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