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arXiv 2104.10052astro-ph.HE
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超新星遗迹和相关脉冲星的定量年龄估算

Quantitative Age Estimation of Supernova Remnants and Associated Pulsars

Hiromasa Suzuki, Aya Bamba, Shinpei Shibata

备注：
14 pages, 5 figures, accepted for publication in ApJ
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摘要：

超新星遗迹的年龄（SNR）无疑是研究其演化的最重要属性之一，但在大多数情况下很难可靠地估计。在这项研究中，我们比较了SNRs的动力学和等离子体年龄及其相关中子星的特征年龄与通常认为可靠的相应SNRs年龄（$t_{\rm r}$）：SNRs的历史和光回波年龄，喷出物结的运动学年龄和相关中子星的运动学年龄（NS）。喷出物结或NS的运动学年龄是它们从爆炸中心到达当前位置所花费的时间。我们使用所有可用的24个系统，其中$t_{\rm r}$已经可用（历史，光回波和喷出物运动学年龄）或可测量（NS运动学年龄）。本文通过定量地确定SNR壳层的几何中心，估算了8个SNR-NS系统的NS运动学年龄。获得的$t_{\rm r}$范围为33岁至$\approx 400$ kyr。我们发现，两个SNR年龄，动力学和等离子体年龄，是一致的$t_{\rm r}$在一个因素的四个，而不同的特征年龄的恒星从$t_{\rm r}$的四个因素以上的一些系统。利用本文中总结的$t_{\rm r}$，我们给出了相关星系的初始自旋周期，这比以前的工作，以及更严格的限制。

英文摘要：

The age of a supernova remnant (SNR) is, though undoubtedly one of the most important properties for study of its evolution, difficult to estimate reliably in most cases. In this study, we compare the dynamical and plasma ages of the SNRs and characteristic ages of their associated pulsars with the corresponding SNRs' ages that are generally thought to be reliable ($t_{\rm r}$): historical and light-echo ages of the SNRs, kinematic ages of the ejecta knots and kinematic ages of the associated neutron stars (NS). The kinematic age of ejecta knots or a NS is the time that they have taken to reach the current positions from the explosion center. We use all of the available 24 systems for which $t_{\rm r}$ is already available (historical, light-echo, and ejecta kinematic ages) or measurable (NS kinematic age). We estimate the NS kinematic ages for eight SNR-NS systems by determining quantitatively the geometric centers of the SNR shells. The obtained $t_{\rm r}$ ranges from 33 yr to $\approx 400$ kyr. We find that the two SNR ages, dynamical and plasma ages, are consistent with $t_{\rm r}$ within a factor of four, whereas the characteristic ages of the pulsars differ from $t_{\rm r}$ by more than a factor of four in some systems. Using the $t_{\rm r}$ summarized in this work, we present the initial spin periods of the associated pulsars, which are more strictly constrained than the previous works, as well.

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