  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.
