Energy release in the crust of an accreting neutron star with realistic compositions of thermonuclear ashes

N.N. Shchechilin, M.E. Gusakov, A.I. Chugunov

Ioffe Institute, Politekhnicheskaya 26, Saint Petersburg 194021, Russia

The deep crustal heating, associated with exothermal nuclear reactions, is believed to be a key parameter for describing the thermal evolution of accreting neutron stars. We present the first thermodynamically consistent calculations of the crustal heating for realistic compositions of thermonuclear ashes. In contrast to previous studies based on the traditional approach, we account for neutron hydrostatic/diffusion (nHD) equilibrium condition imposed by superfluidity of neutrons in a major part of the inner crust and rapid diffusion in the remaining part of the inner crust. We apply a simplified reaction network to model nuclear evolution of various multi-component thermonuclear burning ashes (superburst, KEPLER, and extreme rp-process ashes) in the outer crust and calculate the deep crustal heating energy release Q, parametrized by the pressure at the outer-inner crust interface, Poi. Using the general thermodynamic arguments we set a lower limit on Q, Q ≥ 0.13-0.2 MeV per baryon (an actual value depends on the ash composition and the employed mass model).


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