Speaker
Description
We study the thermal evolution of neutron stars in covariant f(Q) gravity, extending our previous work (Alwan, 2025), by coupling a modified TOV with the BSk21 equation of state to the NSCool thermal evolution calculation for non-linear f(Q) models; logarithmic, exponential, and quadratic. Since f(Q) modifications act purely through stellar structure rather than microphysics, they shift the Direct Urca threshold mass $M_{DU}$ relative to general relativity, thereby moving individual stars between the slow, threshold, and fast cooling regimes. The logarithmic and exponential models shift $M_{DU}$ in either direction depending on the sign of the model parameter beta, while the quadratic model shifts it in only one direction. We discuss how these threshold shifts reshape the predicted cooling curves and compare the resulting trends with the observed sample of isolated neutron stars from Beznogov & Yakovlev (2015).