| Issue |
A&A
Volume 366, Number 2, February I 2001
|
|
|---|---|---|
| Page(s) | 532 - 537 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20000090 | |
| Published online | 15 February 2001 | |
Properties of neutron stars with hyperons in the relativistic mean field theory
1
Department of Astronomy, Nanjing University, Nanjing 210093, PR China
2
IHEP, Chinese Academy of Sciences, Beijing 100039, PR China
Corresponding author: T. Lu, tlu@nju.edu.cn
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 
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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