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

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

2011-10-13

arxiv.org/abs/1110.2861v1

Phys. Rev. C 84, 045804 (2011)

Physics

Nuclear Physics

Nuclear Theory

32 pages, 13 figures

Scientific paper

10.1103/PhysRevC.84.045804

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.

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