破裂脉冲星的X射线观测：孤立的中心致密天体没有避难所
X-ray Observations of Disrupted Recycled Pulsars: No Refuge for Orphaned Central Compact Objects
摘要：
本文报道了P > 20 ms，B_s <3E 10 G的分裂再循环星（DRP）的Chandra X射线测量。这些观察的动机是寻找近似的直系后代。超新星遗迹中的10个中心致密天体（CCO），其中三个与DRP具有相似的时间和磁性，但它们是明亮的热X射线源，与最小的中子星冷却曲线一致。由于没有发现DPR，没有证据表明它们是“孤儿”CCO，即超新星遗迹已经消散的中子星。它们的热X射线光度的上限在log Lx[erg/s] = 31.8-32.8的范围内，这意味着冷却年龄> 1 E4 - 1 E5年，大约是银河系类似体积中大约10个已知CCO年龄的10倍。因此，可以通过该方法检测到的一百个CCO后代的数量级本质上是无线电静默的，或者占据与DRP不同的（P，B_s）参数空间的区域。这激发了一种新的X射线搜索，在具有较大B场的射电星系中寻找孤儿CCO，这可以验证它们的场被超新星喷出物的回落所掩埋，但很快重新生长以加入正常脉冲星种群的理论。
英文摘要：
We present a Chandra X-ray survey of the disrupted recycled pulsars (DRPs), isolated radio pulsars with P > 20 ms and B_s < 3E10 G. These observations were motivated as a search for the immediate descendants of the approx. 10 central compact objects (CCOs) in supernova remnants, three of which have similar timing and magnetic properties as the DRPs, but are bright, thermal X-ray sources consistent with minimal neutron star cooling curves. Since none of the DPRs were detected, there is no evidence that they are "orphaned" CCOs, neutron stars whose supernova remnants has dissipated. Upper limits on their thermal X-ray luminosities are in the range log Lx[erg/s] = 31.8-32.8, which implies cooling ages > 1E4 - 1E5 yr, roughly 10 times the ages of the approximately 10 known CCOs in a similar volume of the Galaxy. The order of a hundred CCO descendants that could be detected by this method are thus either intrinsically radio quiet, or occupy a different region of (P,B_s) parameter space from the DRPs. This motivates a new X-ray search for orphaned CCOs among radio pulsars with larger B-fields, which could verify the theory that their fields are buried by fall-back of supernova ejecta, but quickly regrow to join the normal pulsar population.
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