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, firstname.lastname@example.org
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.