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孤立中子星系统的旋转射电瞬变相与中心致密天体后裔

Rotating Radio Transient Phases of Isolated Neutron Star Systems and Descendants of Central Compact Objects

Ş. Demirok, Ü. Ertan, A. A. Gençali

arXiv 2609.24286首次发表:更新:

AI 中文总结

本研究通过回吸盘模型确定孤立中子星演化中的RRAT相,与观测分布吻合,并预测Calvera类CCO后裔成为长寿射电脉冲星,但诞生率极低。

AI 中文摘要

旋转射电瞬变(RRATs)构成了一类孤立中子星(INS)种群,其特征是零星且短暂的射电暴。在回吸盘模型中,已有研究表明大多数孤立中子星种群在其演化过程中会经历一个RRAT相,而产生这些射电暴的机制可能是内盘穿透光圆柱体导致死亡脉冲星开放磁力线通量在极区增强。为检验这一想法,我们确定了沿孤立中子星家族在周期-周期导数($P$--$\dot{P}$)图上的演化曲线,该机制可能产生的RRAT相。这些RRAT相在$P$--$\dot{P}$图中形成一个RRAT区域,这与已知的RRAT分布一致。利用我们的结果,我们还研究了中心致密天体(CCOs)的后裔。我们估计,类似于三个已测量$P$和$\dot{P}$的CCOs的CCOs不太可能成为射电脉冲星(RPs)。对于最近被确认的CCO——Calvera,情况则相当不同。在该模型中,Calvera类源成为射电脉冲星,其寿命大于$10^{8}$年。事实上,在我们的模型中,Calvera类CCOs后裔演化的$P$--$\dot{P}$图区域存在一个射电脉冲星群。我们还估计它们的诞生率非常低,因此它们的直接后裔目前可能不存在于我们的银河系中。

英文摘要

Rotating radio transients (RRATs) form an isolated neutron star (INS) population characterized by their sporadic and short radio bursts. In the fallback disc model, it was suggested that most INS populations pass through an RRAT phase during their evolution, and the mechanism producing these bursts could be the enhancement of the flux of open magnetic field lines through the poles of dead pulsars due to penetration of the inner disc into the light cylinder. To test this idea, we determine the RRAT phases that could be produced by this mechanism along the evolutionary curves of the INS families on the period-period derivative ($P$--$\dot{P}$ diagram). These RRAT phases form an RRAT region in the $P$--$\dot{P}$ diagram, which is in agreement with the known RRAT distribution. Using our results, we also investigate the descendants of central compact objects (CCOs). We estimate that the CCOs similar to the three CCOs with measured $P$ and $\dot{P}$ are not likely to become radio pulsars (RPs). The situation is rather different for Calvera, a recently identified CCO. In the model, Calvera-like sources become RPs with lifetimes $ > 10^{8}$ yr. Indeed, there is a cluster of RPs in the region of \PPdot~diagram where descendants of Calvera-like CCOs evolve in our model. We also estimate that they have a very low birth rate, and therefore their immediate descendants may not currently exist in our Galaxy.

CommentsAccepted for publication in MNRAS, 10 pages, 4 figures

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