2003/05/31 by A. Y. Potekhin, D. G. Yakovlev, G. Chabrier +2 · 2 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Condensed matter physics #Dipole #High-pressure geophysics and materials #Magnetic field #Neutron star #Physics #Pulsars and Gravitational Waves Research #Superfluidity #astro-ph
paper · pdf · doi:10.1086/376900
published as Astrophys.J. 594 (2003) 404-418 · 15 pages, 12 figures, 2 tables. Corrected title only (v2)
openalex publication_date 2003/08/20 · arxiv created 2003/09/17 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study the thermal structure of neutron stars with magnetized envelopes composed of accreted material, using updated thermal conductivities of plasmas in quantizing magnetic fields, as well as the equation of state and radiative opacities for partially ionized hydrogen in strong magnetic fields. The relation between the internal and local surface temperatures is calculated and fitted by an analytic function of the internal temperature, magnetic field strength, angle between the field lines and the normal to the surface, surface gravity, and the mass of the accreted material. The luminosity of a neutron star with a dipole magnetic field is calculated for various values of the accreted mass, internal temperature, and magnetic field strength. Using these results, we simulate cooling of superfluid neutron stars with magnetized accreted envelopes. We consider slow and fast cooling regimes, paying special attention to very slow cooling of low-mass, superfluid neutron stars. In the latter case, the cooling is strongly affected by the combined effect of magnetized accreted envelopes and neutron superfluidity in the stellar crust. Our results are important for the interpretation of observations of the isolated neutron stars hottest for their age, such as RX J0822-43 and PSR B1055-52.