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We study the quiescent luminosities of accreting neutron stars by a newmechanism as neutrino heating for additional deep crustal heating, where theneutrino heating is produced by charged pions decay from the nuclear collisionson the surface of neutron star during its active accretion. For low massneutron star($\lesssim1.4~M_{\odot}$), as the neutrino heating islittle($\lesssim1$ MeV per accreted nucleon) or there would be no neutrinoheating, the quiescent luminsoity will be not affected or slightly affected.While for massive neutron star ($\gtrsim2~M_{\odot}$), the quiescent luminositywill be enhanced more obviously with neutrino heating in the range 2-6 MeV peraccreted 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 andheavy elements surface are considered. The observations on a hot neutron starsuch as RX J0812.4-3114 can be explained with neutrino heating if the directUrca process is forbidden for a massive star with light elements surface, whichis different from the previous work that the hot observations should beexplained with small mass neutron star and the effect of superfluidity.

Quiescent luminosities of transiently accreting neutron stars with neutrino heating due to charged pion decay