论文标题
部分可观测时空混沌系统的无模型预测
Observational evidence for a spin-up line in the P-Pdot diagram of millisecond pulsars
论文作者
论文摘要
据信，毫秒脉冲星通过从同伴恒星那里获得物质和棱角动量来获得快速旋转。积聚过程的理论建模表明，在周期衍生物（$ p $ - $ \ dot {p} $）中的旋转线图（$ p $ - $ \ dot {p} $）图，在X射线比纳里亚里群岛中的无线电脉冲脉冲和累积中子星人群中起着重要作用。在这里，我们使用143个无线电脉冲星的样本（$ p $ <30 ms）提供了这种旋转线的观察证据。我们还发现，位于经典旋转线附近的PSRS〜J1823 $ - $ 3021A和J1824 $ - $ 2452A与广泛的毫秒脉冲星人一致。最后，我们表明我们的贝叶斯推论方法可以探测物理学，从而可以将约束放在积聚率和磁盘 - 磁层相互作用上。
It is believed that millisecond pulsars attain their fast spins by accreting matter and angular momentum from companion stars. Theoretical modelling of the accretion process suggests a spin-up line in the period-period derivative ($P$-$\dot{P}$) diagram of millisecond pulsars, which plays an important role in population studies of radio millisecond pulsars and accreting neutron stars in X-ray binaries. Here we present observational evidence for such a spin-up line using a sample of 143 radio pulsars with $P$ < 30 ms. We also find that PSRs~J1823$-$3021A and J1824$-$2452A, located near the classic spin-up line, are consistent with the broad population of millisecond pulsars. Finally, we show that our approach of Bayesian inference can probe accretion physics, allowing constraints to be placed on the accretion rate and the disk-magnetosphere interaction.
