论文标题
研究$γ$ -Ray Pulsar J1932+1916及其与Chandra的Pulsar Windra
Studying the $γ$-ray pulsar J1932+1916 and its pulsar wind nebula with Chandra
论文作者
论文摘要
我们报告了Chandra X射线观测值的结果$γ$ ray-raie-Quiet Quiet Pulsar J1932+1916。我们从Suzaku和Swift获得的低空间分辨率数据中证实了Pulsar对应物及其脉冲星云的先前检测。具有更好空间分辨率的Chandra数据解决了Pulsar附近的星云的精细结构，可以将其解释为RAM压力弯曲的喷气机。这个紧凑部分的大小约为30''，它被弱的不对称扩散发射延伸至$ \ $ \ $ 2.8'。脉冲星的X射线光谱，星云的紧凑和延伸部分可以由光子指数分别为0.44、2.34和2.14的幂律模型描述。实际的Pulsar的X射线通量比Suzaku和Swift弱的几倍弱，而Swift则被未解决的星云统治。我们讨论了J1932+1916的可能关联与附近的Supernova Remnant G54.4-0.3。
We report on the results of Chandra X-ray observations of the $γ$-ray radio-quiet pulsar J1932+1916. We confirm the previous detection of the pulsar counterpart and its pulsar wind nebula in X-rays from low spatial resolution data obtained by Suzaku and Swift. The Chandra data with much better spatial resolution resolved the fine structure of the nebula in the pulsar vicinity, which can be interpreted as jets bent by the ram pressure. The size of this compact part is about 30'', and it is surrounded by a weak asymmetric diffusive emission extended up to $\approx$ 2.8'. The X-ray spectra of the pulsar, the compact and extended parts of the nebula can be described by the power-law models with photon indexes of 0.44, 2.34 and 2.14, respectively. The actual pulsar's X-ray flux is several times weaker than it was obtained with Suzaku and Swift where it was dominated by the unresolved nebula. We discuss possible associations of J1932+1916 with the nearby supernova remnant G54.4-0.3.
