Cooling of neutron stars in soft X-ray transients with realistic crust composition
arXiv:2411.14395 · doi:10.1016/j.jheap.2024.11.017
Abstract
Thermal radiation of neutron stars in soft X-ray transients (SXTs) in a quiescent state is believed to be powered by the heat deposited in the stellar crust due to nuclear reactions during accretion. Confronting observations of this radiation with simulations helps to verify theoretical models of the dense matter in neutron stars. We simulate the thermal evolution of the SXTs with theoretical models of the equation of state and composition of the accreted crust. The new family of such models were recently developed within a thermodynamically consistent approach by modeling the nuclear evolution of an accreted matter as it sinks toward the stellar center, starting from representative thermonuclear ash compositions. The crust cooling curves computed with the traditional and modern theory are compared with observations of SXTs MXB 1659-29 and IGR J17480-2446. We show that the new and traditional models of the accreted neutron star crusts are similar in their capability to explain the thermal evolution of neutron stars in SXTs. Both kinds of models require inclusion of additional ingredients not supplied by the current theory, such as the shallow heating and variation of thermal conductivity, to fit observations.
10 pages, 7 figures, JHEAP, accepted
References in corpus (14)
- Thermonuclear (type-I) X-ray bursts observed by the Rossi X-ray Timing Explorer
- Models of crustal heating in accreting neutron stars
- Dependence of X-Ray Burst Models on Nuclear Reaction Rates
- Cooling of Accretion-Heated Neutron Stars
- Cooling of the crust in the neutron star low-mass X-ray binary MXB 1659-29
- Distances of the bulge globular clusters Terzan 5, Liller 1, UKS 1 and Terzan 4 based on HST NICMOS photometry
- Crust structure and thermal evolution of neutron stars in soft X-ray transients
- Thermodynamically consistent equation of state for an accreted neutron star crust
- Deep crustal heating for realistic compositions of thermonuclear ashes
- Thermal evolution of neutron stars in soft X-ray transients with thermodynamically consistent models of the accreted crust
- Fast neutrino cooling in the accreting neutron star MXB 1659-29
- Gapless neutron superfluidity can explain the late time cooling of transiently accreting neutron stars
- Accreting neutron stars: composition of the upper layers of the inner crust
- Gapless neutron superfluidity in the crust of the accreting neutron stars KS 1731-260 and MXB 1659-29