Magnetars as cooling neutron stars with internal heating

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dc.creatorKaminker, A. D.
dc.creatorYakovlev, D. G.
dc.creatorPotekhin, A. Y.
dc.creatorShibazaki, N.
dc.creatorShternin, P. S.
dc.creatorGnedin, O. Y.
dc.date2006-05-18
dc.date.accessioned2026-07-07T10:23:07Z
dc.date.available2026-07-07T10:23:07Z
dc.descriptionWe study thermal structure and evolution of magnetars as cooling neutron stars with a phenomenological heat source in a spherical internal layer. We explore the location of this layer as well as the heating rate that could explain high observable thermal luminosities of magnetars and would be consistent with the energy budget of neutron stars. We conclude that the heat source should be located in an outer magnetar's crust, at densities rho < 5e11 g/cm^3, and should have the heat intensity of the order of 1e20 erg/s/cm^3. Otherwise the heat energy is mainly emitted by neutrinos and cannot warm up the surface.
dc.description8 pages, 5 figures, submitted to MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0605449
dc.identifierhttp://arxiv.org/abs/astro-ph/0605449
dc.identifierMon.Not.Roy.Astron.Soc.371:477-483,2006
dc.identifierdoi:10.1111/j.1365-2966.2006.10680.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175714
dc.subjectAstrophysics
dc.titleMagnetars as cooling neutron stars with internal heating
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