منابع مشابه
Magneto–thermal evolution of neutron stars
Context. The presence of magnetic fields in the crust of neutron stars causes a non-spherically symmetric temperature distribution. The strong temperature dependence of the magnetic diffusivity and thermal conductivity, together with the heat generated by magnetic dissipation, couple the magnetic and thermal evolution of NSs, that cannot be formulated as separated one–dimensional problems. Aims...
متن کاملThermal Evolution of Isolated Neutron Stars
After a brief summary of neutron star cooling theory I present results which emphasize the importance of baryon pairing in the neutron star core. I show how the thermal evolution may be totally controlled by pairing for models which include only nucleons and models containing also hyperons. Finally, I consider the thermal evolution of ultramagnetized neutron stars whose existence has been infer...
متن کاملThe Thermal Evolution of Ultramagnetized Neutron Stars
Using recently calculated analytic and numerical models for the thermal structure of ultramagnetized neutron stars, we estimate the effects that ultrastrong magnetic fields B ≥ 10 G have on the thermal evolution of a neutron star. Understanding this evolution is necessary to interpret models that invoke “magnetars” to account for soft γ-ray emission from some repeating sources. Subject headings...
متن کاملEvolution of Isolated Neutron Stars
Abstract. In this paper we briefly review our recent results on evolution and properties of isolated neutron stars (INSs) in the Galaxy. As the first step we discuss stochastic period evolution of INSs. We briefly discuss how an INS’s spin period evolves under influence of interaction with turbulized interstellar medium. To investigate statistical properties of the INS population we calculate a...
متن کاملNeutron superfluidity in strongly magnetic interiors of neutron stars and its effect on thermal evolution
The possibility of a neutron m = 2–superfluid in the interior of neutron stars is investigated. This pairing state is energetically favoured in strong magnetic fields (H ∼ 10 − 10 G). Because of the node in the angulardependent energy gap along the field direction the neutrino emissivity is only suppressed polynomially as function in T/Tc instead of exponentially, as it is obtained for a nodele...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2009
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:200811229