论文标题
长期Period Pulsar Gleam-X J162759.5-523504.3的演变
Evolution of the long-period pulsar GLEAM-X J162759.5-523504.3
论文作者
论文摘要
在最近发现的Pulsar Gleam-X J162759.5-523504.3中，长期（$ p = 1091 $ s）可以由中子恒星来获得，随着后备光盘和磁性偶极时刻和$ 10^{30} $ g cm $^3 $的磁性二极管的含量超过$ \ sim flim flip $ \ sim 2 $ \ sim 2 \ yr \ sim flim \ sim 2^5 $ y y yrip \ sim flim \ sim flim \ sim flim \ sim 2^5 $ y y yrip \ y y y yrip \ sim times 10^5 $ y yr衍生物，$ \ dot {p} $和X射线光度，$ l_x $，source。 $ \ dot {p} $的当前上限允许两个替代状态：（1）圆盘仍处于较低速度的持续积聚，使积聚的发光度远小于中子星的冷却亮度，又低于$ l_x $的上限。在这种情况下，旋转将继续以$ \ dot {p} \ sim 10^{ - 10} $ s s $^{ - 1} $，直到光盘变得不活跃；最后一个时期将为$ p \ sim $ $ 10^3 $ s。 （2）光盘已经不活跃，没有积聚。在这种情况下，周期的演变已升至最后一个周期范围内观察到的值。剩下的，非常虚弱的偶极扭矩持续渐近旋转以$ \ dot {p} \ sim 4 \ times 10^{ - 18} $ s s $ s $ s $^{ - 1} $。长时间$ p \ sim $ $ 10^3 $ s的最终状态被预测，在与后备碟片模型的早期工作中，软伽玛中继器和异常的X射线脉冲星有相对较强的偶极子场。
The long-period ($P = 1091$ s) of the recently discovered pulsar GLEAM-X J162759.5-523504.3 can be attained by neutron stars evolving with fallback discs and magnetic dipole moments of a few $10^{30}$ G cm$^3$ at ages greater than $\sim 2 \times 10^5$ yr consistently with the observational upper limits to the period derivative, $\dot{P}$, and the X-ray luminosity, $L_X$, of the source. The current upper limits for $\dot{P}$ allow two alternative present states: (1) The disc is still active with ongoing accretion at a low rate such that the accretion luminosity is much less than the neutron star's cooling luminosity, which in turn is below the upper limit for $L_X$. In this scenario the spin-down will continue at $\dot{P} \sim 10^{-10}$ s s$^{-1}$ until the disc becomes inactive; the final period will be $P \sim$ a few $10^3$ s. (2) The disc is already inactive, there is no accretion. In this case the period evolution has leveled off to the observed value in the final period range. The remaining, very weak, dipole torque sustaining asymptotic spin-down at $\dot{P} \sim 4 \times 10^{-18}$ s s$^{-1}$. Long periods $P \sim$ a few $10^3$ s were predicted for the final states of soft gamma repeaters and anomalous X-ray pulsars with relatively strong dipole fields in earlier work with the fallback disc model.
