Transition density and pressure in hot neutron stars

Abstract

Using the momentum-dependent MDI effective interaction for nucleons, we have studied the transition density and pressure at the boundary between the inner crust and liquid core of hot neutron stars. We find that their values are larger in neutrino-trapped neutron stars than in neutrino-free neutron stars. Furthermore, both are found to decrease with increasing temperature of a neutron star as well as increasing slope parameter of the nuclear symmetry energy, except that the transition pressure in neutrino-trapped neutron stars for the case of small symmetry energy slope parameter first increases and then decreases with increasing temperature. We have also studied the effect of the nuclear symmetry energy on the critical temperature above which the inner crust in a hot neutron star disappears and found that with increasing value of the symmetry energy slope parameter, the critical temperature decreases slightly in neutrino-trapped neutron stars but first decreases and then increases in neutrino-free neutron stars.

7 pages, 6 figures, version to appear in Phys. Rev. C

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Cited by in corpus (6)

• Imprints of the nuclear symmetry energy on the tidal deformability of neutron stars
• Thermal properties of asymmetric nuclear matter with an improved isospin- and momentum-dependent interaction
• Study of the core-crust transition in neutron stars with finite-range interactions: the dynamical method
• Density matrix expansion for the MDI interaction
• Mean-field study of hot beta-stable protoneutron star matter: Impact of the symmetry energy and nucleon effective mass
• Dynamical properties of nuclear and stellar matter and the symmetry energy