  We study the quiescent luminosities of accreting neutron stars by a new
mechanism as neutrino heating for additional deep crustal heating, where the
neutrino heating is produced by charged pions decay from the nuclear collisions
on the surface of neutron star during its active accretion. For low mass
neutron star($\lesssim1.4~M_{\odot}$), as the neutrino heating is
little($\lesssim1$ MeV per accreted nucleon) or there would be no neutrino
heating, the quiescent luminsoity will be not affected or slightly affected.
While for massive neutron star ($\gtrsim2~M_{\odot}$), the quiescent luminosity
will be enhanced more obviously with neutrino heating in the range 2-6 MeV per
accreted nucleon. The observations on cold neutron stars such as 1H 19605+00,
SAX J1808.4-3658 can be explained with neutrino heating if a fast cooling and
heavy elements surface are considered. The observations on a hot neutron star
such as RX J0812.4-3114 can be explained with neutrino heating if the direct
Urca process is forbidden for a massive star with light elements surface, which
is different from the previous work that the hot observations should be
explained with small mass neutron star and the effect of superfluidity.
