Neutrino Emission of Neutron-Star Superbursts

Superbursts of neutron stars are rare but powerful events explained by the explosive burning
of carbon in the deep layers of the outer envelope of the star. In this paper we perform a simulation of
superbursts and propose a simple method for describing the neutrino stage of their cooling, as well as a
method for describing the evolution of the burst energy on a scale of several months. We note a universal
relation for the temperature distribution in the burnt layer at its neutrino cooling stage, as well as the
unification of bolometric light curves and neutrino heat loss rates for deep and powerful bursts. We point
out the possibility of long-term retention of the burst energy in the star’s envelope. The results can be useful
for interpretation of superburst observations.