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We study the effect of physics input on thermal evolution of neutron stars insoft X-ray transients (SXTs). In particular, we consider different modernmodels of the sources of deep crustal heating during accretion episodes and theeffects brought about by impurities embedded in the crust during its formation.We simulate thermal structure and evolution of episodically accreting neutronstars under different assumptions on the crust composition and on thedistribution of heat sources and impurities. For the nonaccreted crust, weconsider the nuclear charge fluctuations that arise at crust formation. For theaccreted crust, we compare different theoretical models of composition andinternal heating. We also compare results of numerical simulations withobservations of the crust cooling in SXT MXB 1659-29. We found that thenonaccreted part of the inner crust of a neutron star can have a layeredstructure, with almost pure crystalline layers interchanging with layerscomposed of mixtures of different nuclei. The latter layers have relatively lowthermal conductivities, which affects thermal evolution of the transients. Theimpurity distribution in the crust strongly depends on the models of the densematter and the crust formation scenario. The shallow heating that is needed toreach agreement between the theory and observations depends on characteristicsof the crust and envelope.

Crust structure and thermal evolution of neutron stars in soft X-ray transients