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首页> 外文期刊>The Astrophysical journal >Deep Chandra Observation Of The Pulsar Wind Nebula Powered By Pulsar Psr J1846-0258 Tn The Supernova Remnant Kes 75
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Deep Chandra Observation Of The Pulsar Wind Nebula Powered By Pulsar Psr J1846-0258 Tn The Supernova Remnant Kes 75

机译：由Pulsar Psr J1846-0258供电的脉冲星云的深Chandra观测超新星遗迹Kes 75

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摘要

We present the results of detailed spatial and spectral analysis of the pulsar wind nebula (PWN) in supernova remnant Kes 75 (G29.7-0.3) using a deep exposure with Chandra X-Ray Observatory. The PWN shows a complex morphology with clear axisymmetric structure. We identified a one-sided jet and two bright clumps aligned with the overall nebular elongation, and an arclike feature perpendicular to the jet direction. We interpret the arc as an equatorial torus or wisp and the clumps could be shock interaction between the jets and the surrounding medium. Spatial modeling of the features with a torus and jet model indicates a position angle 207°± 8° for the PWN symmetry axis. The lack of any observable counter jet implies a flow velocity larger than 0.4 c. Comparing to an archival observation 6 yr earlier, some small-scale features in the PWN demonstrate strong variability: the flux of the inner jet doubles, and the peak of the northern clump broadens and shifts 2" outward. As recently reported from RXTE observations, magnetar-like bursts of the central pulsar occurred coincidentally 7 days before the Chandra exposure. Accompanied with the bursts is a temporary increase in the pulsar flux: during the Chandra observation, the pulsar luminosity is 6 times larger than in quiescent state, and shows substantial spectral softening from Г = 1.1 to 1.9 with an emerging thermal component.
机译：我们使用Chandra X射线天文台进行深度曝光，对超新星残余Kes 75（G29.7-0.3）中的脉冲星云（PWN）进行了详细的空间和光谱分析，得出了结果。 PWN具有复杂的形态，具有清晰的轴对称结构。我们确定了一个单侧射流和两个明亮的团块，它们与整个星云的延伸方向对齐，并且具有垂直于射流方向的弧形特征。我们将弧线解释为赤道圆环或小束，而团块可能是喷流与周围介质之间的震动相互作用。使用环面和喷射模型对特征进行空间建模表明，PWN对称轴的位置角为207°±8°。缺少任何可观察到的反向射流意味着流速大于0.4 c。与6年前的档案观测相比，PWN的一些小尺度特征显示出强烈的可变性：内部射流的通量增加了一倍，北部丛的峰变宽并向外移动了2“。正如RXTE观测最近报道的那样，在Chandra暴露之前的第7天，中心脉冲星的磁脉冲状爆发同时发生，伴随着脉冲爆发，脉冲星通量暂时增加：在Chandra观测期间，脉冲星的发光度是静止状态下的6倍，并且显示出随着新出现的热分量，光谱从Г= 1.1变到1.9。

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