Thermalization time and specific heat of the neutron stars crust
Por:
Fortin M., Grill F., Margueron J., Page D., Sandulescu N.
Publicada:
27 dic 2010
Categoría:
Nuclear and High Energy Physics
Resumen:
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.
Filiaciones:
Fortin M.:
Institut de Physique Nucléaire, IN2P3-CNRS, Université Paris-Sud, F-91406 Orsay Cedex, France
Icole Normale Supérieure, Departement de Physique, 24 rue Lhomond, F-75005 Paris, France
Grill F.:
Dipartimento di Fisica, Universitá Degli Studi di Milano, Via Celoria 16, I-20133 Milan, Italy
Margueron J.:
Institut de Physique Nucléaire, IN2P3-CNRS, Université Paris-Sud, F-91406 Orsay Cedex, France
Page D.:
Univ Nacl Autonoma Mexico, Dept Astrofis Teor, Astron Inst, Mexico City 04360, DF, Mexico
Sandulescu N.:
National Institute of Physics and Nuclear Engineering, RO-76900 Bucharest, Romania
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