Speaker
Description
The present study explores the thermal evolution and emission properties of neutron stars by combining $f(R,T)$-modified equilibrium stellar backgrounds with the NSCool cooling framework. We compute stellar mass and pressure profiles by solving the Tolman-Oppenheimer-Volkoff equations in both Einstein gravity and modified gravity by employing the APR, FPS, and SLy equations of state. Using these profiles as input to the standard NSCool, the study assesses the redshifted photon ($L_\gamma^\infty$) as well as surface temperature ($T_s^{\infty}$) for neutron stars with $1.4 \rm M_\odot$. It quantifies their dependence and sensitivity on the modified-gravity parameter ($\lambda$), equations of state, and the adopted microphysical inputs. Our results show that the modified-gravity parameter shifts the cooling and luminosity tracks relative to general relativity. It suggests that the interpretation of these shifts must be considered alongside standard-cooling uncertainties, in particular nucleon pairing (superfluidity) and the envelope $T_s$-$T_b$ relation. These findings on redshifted photon luminosities $L_\gamma^\infty$ and surface temperature $T_s^{\infty}$ are discussed in the context of available temperature and luminosity observations.