Deep crustal heating for realistic compositions of thermonuclear ashes

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. In this paper, 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 (nal)) 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, P-oi. 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).

Automated summary

This study presents the first thermodynamically consistent calculations of crustal heating for realistic compositions of thermonuclear ashes, taking into account neutron superfluidity and rapid diffusion effects. A simplified reaction network is used to model nuclear evolution, leading to a lower limit for the deep crustal heating energy release, while the actual value depends on the ash composition and used mass model.