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 ($\lesssim 1.4M_{\odot }$), as the neutrino heating is little ($\lesssim 1\mathrm{MeV}$ per accreted nucleon) or there would be no neutrino heating, the quiescent luminosity will be not affected or slightly affected. While for massive neutron star ($\gtrsim 2M_{\odot }$), 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.

中文翻译：

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由于带电介子衰变导致中微子加热的瞬态吸积中子星的静态光度

我们通过一种新机制来研究吸积中子星的静态光度，即中微子加热用于额外的深层地壳加热，其中中微子加热是由中子星活跃吸积过程中表面核碰撞产生的带电介子衰变产生的。对于低质量中子星（$\lesssim 1.4{米}_{\odot }$), 因为中微子加热很小 ($\lesssim 1\mathrm{兆电子伏}$每个吸积核子）或不会有中微子加热，静态光度不会受到影响或受到轻微影响。而对于大质量中子星（$\gtrsim 2{米}_{\odot }$)，每个吸积核子在 2-6 MeV 范围内加热中微子时，静态光度将得到更明显的增强。1H等冷中子星的观测$19605+00$, 如果考虑快速冷却和重元素表面，SAX J1808.4-3658 可以用中微子加热来解释。RX J0812.4-3114等热中子星的观测，如果对轻元素表面的大质量恒星禁止直接Urca过程，就可以用中微子加热来解释，这不同于以往的热观测应该是用小质量中子星和超流的作用来解释。