Speaker
Description
Motivated by theoretical inquiries into the effective capture of dark matter by neutron stars, this study delves into the potential indirect impacts of captured dark matter on the cooling process of a neutron star. Utilizing the relativistic mean-field formalism with the IOPB-I parameter set, we derive the equation of states for various configurations of dark matter-admixed stars at finite temperatures. Our findings reveal significant alterations in neutrino emissivity, influenced by variations in dark matter momentum and specific neutrino-generating processes within the star. We also investigate the specific heat and thermal conductivity of dark matter-admixed stars to understand the propagation of cooling waves within the star's interior. The study explores the correlation between theoretical surface temperature cooling curves, equation of state, chemical composition of stellar matter, and observational thermal radiation data from diverse sources. Notably, we observe that dark matter-admixed canonical stars with dark matter momentum exceeding 0.04 adhere to a fast cooling scenario. Additionally, we calculate the metric for the internal thermal relaxation epoch with different dark matter momentum, concluding that an increase in the dark matter segment amplifies the cooling and internal relaxation rates of the star.
