Magnetars as cooling neutron stars with internal heating
arXiv:astro-ph/0605449 · doi:10.1111/j.1365-2966.2006.10680.x
Abstract
We 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.
8 pages, 5 figures, submitted to MNRAS
Cited by in corpus (7)
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- Pulsars as Astrophysical Laboratories for Nuclear and Particle Physics
- Evidence for Heating of Neutron Stars by Magnetic Field Decay
- Heating and cooling of magnetars with accreted envelopes
- Origin and evolution of magnetars
- Cooling of Neutron Stars with Strong Toroidal Magnetic Fields
- Joule heating in high magnetic field pulsars