Thermal structure and cooling of neutron stars with magnetized envelopes
Abstract
The thermal structure of neutron stars with magnetized envelopes is studied using modern physics input. The relation between the internal (T_i) and local surface temperatures is calculated and fitted by analytic expressions for magnetic field strengths B from 0 to 10^{16} G and arbitrary inclination of the field lines to the surface. The luminosity of a neutron star with dipole magnetic field is calculated and fitted as a function of B, T_i, stellar mass and radius. In addition, we simulate cooling of neutron stars with magnetized envelopes. In particular, we analyse ultramagnetized envelopes of magnetars and also the effects of the magnetic field of the Vela pulsar on the determination of critical temperatures of neutron and proton superfluids in its core.
Cite
@article{arxiv.astro-ph/0105261,
title = {Thermal structure and cooling of neutron stars with magnetized envelopes},
author = {A. Y. Potekhin and D. G. Yakovlev},
journal= {arXiv preprint arXiv:astro-ph/0105261},
year = {2007}
}
Comments
14 pages, 1 table, 11 figures, LaTeX2e using aa.cls (included) and epsf.sty. Accepted by A&A. Proof-stage version: minor text corrections and one correction of an in-line formula