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The cooling process of a protoneutron star is investigated with focus on itssensitivity to properties of hot and dense matter. An equation of state, whichincludes the nucleon effective mass and nuclear symmetry energy at twice thesaturation density as control parameters, is constructed for systematicstudies. The numerical code utilized in this study follows a quasi-staticevolution of a protoneutron star solving the general-relativistic stellarstructure with neutrino diffusion. The cooling timescale evaluated from theneutrino light curve is found to be longer for the models with larger effectivemasses and smaller symmetry energies at high densities. The present results arecompared with those for other equations of state and it is found that they areconsistent in terms of their dependences on the effective mass and neutron starradius.

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