We investigate the evolution of the surface properties of models for rotating massive stars, i.e., their luminosities, effective temperatures, surface rotational velocities, and surface abundances of all isotopes, from the zero age main sequence to the supernova stage. Our results are based on the grid of stellar models by Heger et al. (2000), which covers solar metallicity stars in the initial...

We study the influence of the symmetry energy of the equation of state on the thermal evolution of protoneutron stars and the properties of supernova neutrinos by the numerical simulations after the protoneutron stars are formed. As for the equation of state (EOS) of nuclear matter, we take two EOS’s with different symmetry energies obtained by the relativistic mean field theory. We find the sy...

Aims. We investigate the influence of high–energy stellar radiation at close–in orbits on atmospheric mass loss during stellar evolution of a G–type star. Methods. High–energy stellar luminosity varies over a wide range for G field stars. The temporal evolution of the distribution of stellar X–ray luminosity and its influence on the evolution of close–in exoplanets is investigated. X–ray lumino...