par Pastore, Alessandro 
;Chamel, Nicolas ;Margueron, Jérôme
Référence Monthly notices of the Royal Astronomical Society, 448, page (1187-1892)
Publication Publié, 2015-02-21
;Chamel, Nicolas ;Margueron, JérômeRéférence Monthly notices of the Royal Astronomical Society, 448, page (1187-1892)
Publication Publié, 2015-02-21
Article révisé par les pairs
| Résumé : | The heat capacity of neutron matter is studied over the range of densities and temperatures prevailing in neutron-star crusts, allowing for the transition to a superfluid phase at temperatures below some critical temperature $T_{sf}$ and including the transition to the classical limit. Finite temperature Hartree-Fock-Bogoliubov equations (FTHFB) are solved and compared to existing approximate expressions. In particular, the formula given by Levenfish and Yakovlev is found to reproduce the numerical results with a high degree of accuracy for temperatures $Tleq T_{sf}$. In the non-superfluid phase, $Tgeq T_{sf}$, the linear approximation is valid only at temperature $Tll T_{{m F} n}$ ($T_{{m F} n}$ being the Fermi temperature of the neutron gas) which is rarely the case in the shallow layers of the neutron star's crust. A non-perturbative interpolation between the quantal and the classical regimes is proposed here. The heat capacity, conveniently parametrized solely in terms of $T_{sf}$, $T_{{m F} n}$, and the neutron number density $n_n$, can be easily implemented in neutron-star cooling simulations. |
