Pasta phases in neutron star studied with extended relativistic mean field models

Abstract

To explain several properties of finite nuclei, infinite matter, and neutron stars in a unified way within the relativistic mean field models, it is important to extend them either with higher order couplings or with density-dependent couplings. These extensions are known to have strong impact in the high-density regime. Here we explore their role on the equation of state at densities lower than the saturation density of finite nuclei which govern the phase transitions associated with pasta structures in the crust of neutron stars.

Accepted in Phys Rev. C 2013

References in corpus (4)

• Neutron-Rich Nuclei in Heaven and Earth
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Isotopic dependence of the giant monopole resonance in the even-A ^{112-124}Sn isotopes and the asymmetry term in nuclear incompressibility
• Role of higher order couplings in the presence of kaons in relativistic mean field description of neutron stars

Cited by in corpus (8)

• Nuclear Waffles
• Unified neutron star EOSs and neutron star structures in RMF models
• Impact of the neutron-star deformability on equation of state parameters
• Nuclear pasta structures and symmetry energy
• Unified nuclear matter EOSs constrained by the in-medium balance in density-dependent covariant density functionals
• Nuclear pasta structures at high temperatures
• Properties and microscopic structures of dense stellar matter in RMF models
• Correlation between the curvature and some properties of the neutron star