Heating and cooling of magnetars with accreted envelopes

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dc.creatorKaminker, A. D.
dc.creatorPotekhin, A. Y.
dc.creatorYakovlev, D. G.
dc.creatorChabrier, G.
dc.date2009-02-24
dc.date.accessioned2026-07-07T13:16:20Z
dc.date.available2026-07-07T13:16:20Z
dc.descriptionWe 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.
dc.description13 pages, 10 figures, 5 tables, accepted for publication in MNRAS
dc.identifierhttps://arxiv.org/abs/0902.4213
dc.identifierhttp://arxiv.org/abs/0902.4213
dc.identifierMNRAS 395 (2009) 2257-2267
dc.identifierdoi:10.1111/j.1365-2966.2009.14693.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/230759
dc.subjectSolar and Stellar Astrophysics
dc.titleHeating and cooling of magnetars with accreted envelopes
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