2001/05/31 by A. Y. Potekhin, D. G. Yakovlev · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Pulsars and Gravitational Waves Research #Scientific Research and Discoveries #astro-ph
paper · pdf · doi:10.1051/0004-6361:20010698
published as Astron.Astrophys. 374 (2001) 213-226 · 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
arxiv created 2001/06/19 · openalex publication_date 2001/07/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
The thermal structure of neutron stars with magnetized envelopes is studied using modern physics input. The relation between the internal () and local surface temperatures is calculated and fitted by analytic expressions for magnetic field strengths B from 0 to 1016 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, , 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.