Temperature and density dependence of asymmetric nuclear matter and protoneutron star properties within an extended relativistic mean field model

Abstract

The effect of temperature and density dependence of the asymmetric nuclear matter properties is studied within the extended relativistic mean field (ERMF) model, which includes the contribution from the self and mixed interaction terms by using different parametrizations obtained by varying the neutron skin thickness $\Delta$r and $\omega$-meson self-coupling ($\zeta$). We observed that the symmetry energy and its slope and incompressibility coefficients decrease with increasing temperatures up to saturation densities. The ERMF parametrizations were employed to obtain a new set of equations of state (EOS) of the protoneutron star (PNS) with and without inclusion of hyperons. In our calculations, in comparison with cold compact stars, we obtained that the gravitational mass of the protoneutron star with and without hyperons increased by $\sim 0.4M_{\odot }$ and its radius increased by $\sim 3$km. Whereas in case of the rotating PNS, the mass shedding limit decreased with increasing temperature, and this suggested that the keplerian frequency of the PNS, at T = 10 MeV should be smaller by $14-20$ for the EOS with hyperon, as compared to the keplerian frequency of a cold compact star.

32 pages, 13 figures

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Cited by in corpus (5)

• Extended Skyrme interactions for nuclear matter, finite nuclei and neutron stars
• Isoscalar-vector interaction and hybrid quark core in massive neutron stars
• Critical parameters of consistent relativistic mean-field models
• Nuclear symmetry energy and the role of three-body forces
• Temperature effects on the neutron matter equation of state obtained from chiral effective field theory