Heating and cooling of magnetars with accreted envelopes

Details Heating and cooling of magnetars with accreted envelopes Heating and cooling of magnetars with accreted envelopes

2009-02-24

arxiv.org/abs/0902.4213v1

MNRAS 395 (2009) 2257-2267

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

13 pages, 10 figures, 5 tables, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2009.14693.x

We study the thermal structure and evolution of magnetars as cooling neutron stars with a phenomenological heat source in an internal layer. We focus on the effect of magnetized (B > 10^{14} G) non-accreted and accreted outermost envelopes composed of different elements, from iron to hydrogen or helium. We discuss a combined effect of thermal conduction and neutrino emission in the outer neutron star crust and calculate the cooling of magnetars with a dipole magnetic field for various locations of the heat layer, heat rates and magnetic field strengths. Combined effects of strong magnetic fields and light-element composition simplify the interpretation of magnetars in our model: these effects allow one to interpret observations assuming less extreme (therefore, more realistic) heating. Massive magnetars, with fast neutrino cooling in their cores, can have higher thermal surface luminosity.

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