Volume 416, Number 3, March IV 2004
|Page(s)||1013 - 1022|
|Section||Stellar structure and evolution|
|Published online||09 March 2004|
Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars
N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland e-mail: firstname.lastname@example.org
2 LUTH, UMR 8102 du CNRS, Observatoire de Paris, 92195 Meudon Cedex, France e-mail: email@example.com;Eric.Gourgoulhon@obspm.fr
Corresponding author: J. L. Zdunik, firstname.lastname@example.org
Accepted: 12 November 2003
The effect of the hyperon softening of the equation of state (EOS) of dense matter on the spin evolution of isolated neutron stars is studied for a broad set of hyperonic EOSs. We use a multidomain 2-D code based on a spectral method, and show how important the precision of solving the equations of stationary motion is for the stability analysis. For some EOSs, the hyperon softening leads to spin-up by angular momentum loss, in the form of the back-bending phenomenon, for a rather broad range of stellar baryon mass. We show that large segments of the evolutionary tracks exhibiting the back-bending behaviour in the moment-of-inertia – rotation-frequency plane are unstable and therefore not astrophysically relevant. We show also that during the spin-up – angular-momentum-loss epoch, an isolated neutron star (e.g. a radio pulsar) can lose a sizable part of its initial angular momentum without significantly changing its rotation period. We propose also simple arguments and criteria allowing one to connect the presence of a back-bending epoch with the mass-radius relations and the stiffness and/or softness of the nucleon and hyperon EOSs of the neutron star core.
Key words: dense matter / equation of state / stars: neutron / stars: rotation
© ESO, 2004
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