卡尔韦拉的演化及类卡尔韦拉中央致密天体的后代

中文摘要 AI 辅助

卡尔韦拉（1RXS J141256.0+792204）是一颗孤立中子星，最近因与超新星遗迹候选体G118.4+37.0相关联而被归类为中央致密天体（CCO）。在这项工作中，我们在回落盘模型中研究了卡尔韦拉以及具有相似初始条件的CCO的长期演化和后代。我们表明，在中子星年龄约为10^4年时，其极区磁场强度约为4×10^10 G时，可以同时再现卡尔韦拉观测到的自旋周期、周期导数和X射线光度，这与该源估计的超新星遗迹年龄一致。在模型中，缺乏普通射电脉冲是由于恒星持续吸积物质。通过模拟，我们估计该源在吸积终止后将成为一颗普通射电脉冲星（RP）。在盘失活后，该源将仅在弱偶极扭矩作用下作为RP长时间（约10^8年）自旋减慢。我们发现，大多数初始条件与卡尔韦拉相似的CCO在其盘失活后也会成为RPs，并且在脉冲星死亡谷的上边界之上或附近。在周期 - 周期导数图中，在我们模型中估计类卡尔韦拉CCO后代所在的区域确实有一群RPs。

英文摘要

Calvera (1RXS J141256.0+792204) is an isolated neutron star recently classified as a central compact object (CCO) after its association with the supernova remnant (SNR) candidate G118.4+37.0. In this work, we investigate the long-term evolution and descendants of Calvera and the CCOs with similar initial conditions in the fallback disc model. We show that the observed spin period, period derivative, and X-ray luminosity of Calvera can be reproduced simultaneously with a magnetic field strength of $\simeq 4 \times 10^{10}$ G at the pole of the neutron star at an age of $\sim 10^4$ yr which is consistent with the estimated SNR age of the source. In the model, the lack of ordinary radio pulsations is due to ongoing mass accretion on to the star. From our simulations, we estimate that the source will become an ordinary radio pulsar (RP) after the termination of the accretion. The source will spin down under the weak dipole torque alone as an RP for a very long time ($\gtrsim 10^8$ yr) after the inactivation of the disc. From our simulations, we find that most of the CCOs with initial conditions similar to those of Calvera also become RPs which remain above or close to the upper border of the pulsar death valley after the inactivation of their discs. In the period-period derivative diagram, there is indeed a cluster of RPs in the region where the descendants of Calvera-like CCOs are estimated to be located in our model.

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6 pages, 2 figures, accepted for publication in MNRAS