Cooling timescale for protoneutron stars and properties of nuclear matter: Effective mass and symmetry energy at high densities

Abstract

The cooling process of a protoneutron star is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a protoneutron star solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.

11 pages, 9 figures, accepted for publication in ApJ

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Cited by in corpus (19)

• Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817
• Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
• Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions
• Three-dimensional simulation of a core-collapse supernova for a binary star progenitor of SN 1987A
• Universal relation for supernova gravitational waves
• EoS for hot neutron stars
• Protoneutron Star Convection Simulated with a New General Relativistic Boltzmann Neutrino Radiation-Hydrodynamics Code
• Probing high-density nuclear symmetry energy with ${\Xi }^{-}/{\Xi }^0$ ratio in heavy-ion collisions at $\sqrt{s_{NN}}\sim 3$ GeV
• Observing Supernova Neutrino Light Curves with Super-Kamiokande. II. Impact of the Nuclear Equation of State
• Efficient estimation method for time evolution of proto-neutron star mass and radius from supernova neutrino signal
• Leptonic and semi-leptonic neutrino interactions with muons in the proto-neutron star cooling
• Effects of nuclear matter and composition in core-collapse supernovae and long-term proto-neutron star cooling
• Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos
• Influence of effective nucleon mass on equation of state for supernova simulations and neutron stars
• Detectability of Late-time Supernova Neutrinos with Fallback Accretion onto Protoneutron star
• Equation of state and neutrino transfer in supernovae and neutron stars
• Influence of the effective mass on the properties of nuclear matter at finite density and temperature
• Simple fits for the neutrino luminosities from protoneutron star cooling
• Role of symmetry energy at subnuclear densities in protoneutron star crusts