Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction

Abstract

The equation of state of hot neutron star matter of n+p+e+$\mu$ composition in $\beta$-equilibrium is studied for both neutrino-free isothermal and neutrino-trapped isentropic conditions, using the formalism where the thermal evolution is built upon its zero-temperature predictions in a self-consistent manner. The accuracy of the parabolic approximation, often used in the finite temperature calculation of hot neutron star matter, is verified by comparing with the results obtained from the exact evaluation in the neutrino-free neutron star matter. The equation of state of neutrino-trapped isentropic matter at low entropic condition, relevant to the core-collapsing supernovae, is formulated. In the isentropic matter, the particle fractions and equation of state have marginal variance as entropy per particle varies between 1 to 3 (in the unit of k${}_B$), but the temperature profile shows marked variation. The isentropes are found to be much less sensitive to the nuclear matter incompressibility, but have a large dependence on the slope parameter L. The bulk properties of the neutron stars predicted by the isentropic equation of state for different entropy are calculated. A model calculation for the early stage evolution of the protoneutron star to neutron star configuration is also given.

30 pages, 11 figures, submitted to Journal of Physics G

References in corpus (18)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Testing Approximations of Thermal Effects in Neutron Star Merger Simulations
• High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars
• Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
• Properties of hypermassive neutron stars formed in mergers of spinning binaries
• A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
• A Second Relativistic Mean Field and Virial Equation of State for Astrophysical Simulations
• Importance of cooling in triggering the collapse of hypermassive neutron stars
• Hot quark matter and (proto-) neutron stars
• Microscopic equation of state of hot nuclear matter for numerical relativity simulations
• Probing the incompressibility of nuclear matter at ultra-high density through the prompt collapse of asymmetric neutron star binaries
• Massive hybrid stars with a first order phase transition
• Effects of isospin and momentum dependent interactions on liquid-gas phase transition in hot asymmetric nuclear matter
• Magnetic susceptibility and magnetization properties of asymmetric nuclear matter under a strong magnetic field
• Correlations between charge radii differences of mirror nuclei and stellar observables
• Study of spin polarized nuclear matter and finite nuclei with finite range simple effective interaction

Cited by in corpus (2)

• $f$ and $p$ mode oscillation of proto-neutron stars with systematic variation of the nucleon effective mass
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