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Thermalization time and specific heat of the neutron stars crust

Abstract : We discuss the thermalization process of the neutron star's crust described by solving the heat-transport equation with a microscopic input for the specific heat of baryonic matter. The heat equation is solved with initial conditions specific to a rapid cooling of the core. To calculate the specific heat of inner-crust baryonic matter, that is, nuclear clusters and unbound neutrons, we use the quasiparticle spectrum provided by the Hartree-Fock-Bogoliubov approach at finite temperature. In this framework, we analyze the dependence of the crust thermalization on pairing properties and on cluster structure of inner-crust matter. It is shown that the pairing correlations reduce the crust thermalization time by a large fraction. The calculations show also that the nuclear clusters have a non-negligible influence on the time evolution of the surface temperature of the neutron star
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Contributor : Sophie Heurteau <>
Submitted on : Wednesday, March 9, 2011 - 3:44:38 PM
Last modification on : Friday, July 2, 2021 - 3:39:22 AM

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M. Fortin, F. Grill, J. Margueron, D. Page, N. Sandulescu. Thermalization time and specific heat of the neutron stars crust. Physical Review C, American Physical Society, 2010, 82, pp.065804. ⟨10.1103/PhysRevC.82.065804⟩. ⟨in2p3-00575105⟩



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