Thermal X‐Ray Pulses Resulting from Pulsar Glitches

Abstract

The non-spherical symmetric transport equations and exact thermal evolution model are used to calculate the transient thermal response to the pulsar’s glitches. The three ways of energy release originated from glitches, namely the ‘shell’, ‘ring’ and ‘spot’ cases are compared. Their luminosity profiles for various sets of parameters are computed. The ‘ ring ’ case is always the middle one in terms of the response time, the response duration and the intensity of the response. This is not unexpected as the volume in which glitch energy is released in the ‘ ring ’ case is between those of the ‘shell’ case and the ‘spot’ case. The effects of initial core temperature before glitch, the density at which the glitch occurs, the amount of energy released in a glitch and the equations of state on the luminosity profiles are also compared.