Thermal Conductivity in Two Regions of a Neutron Star
Recent X-ray observational results1 put fairly stringent upper limits on the blackbody temperatures of compact sources in supernova remnants. For a few seconds during the collapse of a supernova the single star may become as luminous as an entire galaxy containing a trillion stars. One class of highly condensed objects that are believed to be left behind in a supernova collapse are neutron stars. If born in this violent fashion, neutron stars are extremely hot initially, although they cool down quickly due to the profuse emission of energetic neutrinos. Once they are produced in collisions of nucleons or electrons, the weakly-interacting neutrinos have little problem escaping from the star (except perhaps in the first few hundred seconds2). Neutrinos thus lead to a direct local cooling of the interior stellar matter in contrast to cooling due to photons, which is diffusive and radiative from the surface.
KeywordsNeutron Star Effective Thermal Conductivity Supernova Remnant Impurity Diffusion Electron Thermal Conductivity
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