Temperature Effects on Core g-Modes of Neutron Stars

Neutron stars provide a unique physical laboratory in which to study the properties of matter at high density and temperature. We study a diagnostic of the composition of high-density matter, namely, g-mode oscillations, which are driven by buoyancy forces. These oscillations can be excited by tidal forces and couple to gravitational waves. We extend prior results for the g-mode spectrum of cold neutron star matter to high temperatures that are expected to be achieved in neutron star mergers using a parameterization for finite-temperature effects on equations of state recently proposed by Raithel, Ozel and Psaltis. We find that the g-modes of canonical mass neutron stars (approximate to 1.4M(circle dot)) are suppressed at high temperatures, and core g-modes are supported only in the most massive (>= 2M(circle dot)) of hot neutron stars.