Effects of temperature on g-mode oscillations of neutron stars

We investigate finite temperature nuclear matter within the SU(2) chiral sigma model to construct an equation of state relevant for proto-neutron stars. By numerically solving the TOV equations, we obtained macroscopic observables such as mass and radius for various entropy/baryon ratios. We calculate the equilibrium and the adiabatic sound speeds, which encode information regarding the buoyancy of the matter inside the star. From this, we compute the g-mode oscillation spectrum of the star within the relativistic Cowling approximation. We find that the g-modes are suppressed as the entropy of the star increases, which has interesting implication for gravitational wave signals from neutron stars.