标题： 脉冲星的超长周期无线电起源 显示英文标题

标题： A binary origin of ultra-long period radio pulsars

摘要： 我们提出了一种可能的双星演化模型，用于解释超长周期脉冲星（ULPPs）的形成。 该模型包括两个关键阶段：首先，宽距双星中的中子星（NS）通过从其大质量恒星伴星吸积物质而经历有效的自转减速阶段；其次，伴星的超新星爆炸导致双星系统被破坏，并产生两颗孤立的致密星。 其中一个是第一代形成的、缓慢旋转的中子星，我们的双星和自转演化计算表明，自转周期范围从$\lesssim 0.1$秒到$\gtrsim 10^8$秒。这为一些长周期射电暂现源提供了可能的形成途径。 我们估计，银河系中此类系统的形成率大约为$10^{-6}$ $\rm yr^{-1}$ 。 显示英文摘要

摘要： We propose a possible binary evolution model for the formation of ultra-long period pulsars (ULPPs). The model involves two key stages: first, a neutron star (NS) in wide binaries undergoes an effective spin-down phase through wind-fed accretion from its massive stellar companion; second, the supernova explosion of the companion leads to the disruption of the binary system, and produces two isolated compact stars. One of the them is the first-born, slowly rotating NSs, and our binary and spin evolution calculations show that the spin periods range from $\lesssim 0.1$ s to $\gtrsim 10^8$ s. This offers a possible formation channel for some of the long-period radio transients. We estimate that the formation rate of such systems in the Milky Way is approximately about $10^{-6}$ $\rm yr^{-1}$.