论文标题
PSR J1016-5857的“鹅”脉冲星云：Plerion的诞生
"The Goose" Pulsar Wind Nebula of PSR J1016-5857: The Birth of a Plerion
论文作者
论文摘要
我们报告了由年轻的Pulsar PSR PSR J1016--5857提供动力的脉冲星云（PWN）的X射线（CXO）和无线电（ATCA）的结果，我们将其配音为“鹅” PWN。在这两个频段中，图像揭示了尾巴状的PWN形态，这可以归因于Pulsar的运动。通过比较档案和新的CXO观测值，我们测量了Pulsar的正确运动$μ= 28.8 \ PM7.3 $ MAS/YR，产生了一个投影的Pulsar Velocity $ V \约440 \ PM110 $ km/s（d = 3.2 kpc）;它的方向与PWN形状一致。来自PWN的无线电发射是极化的，磁场沿着脉冲星的尾部定向。无线电尾巴连接到较大的无线电结构（在X射线中看不到），我们将其解释为遗物PWN（也称为Plerion）。 CXO数据的频谱分析表明，PWN光谱从$γ= 1.7 $ to $γ\ $γ\ 2.3-2.5 $随着距离Pulsar的距离的增加而软化。软化可以归因于快速的同步加速器燃烧，这将解释较老的遗物PWN缺乏X射线发射。除了非热PWN发射外，我们还从热等离子体中检测到热发射，我们将其归因于宿主SNR。 PULSAR的无线电PWN形态和正确的运动表明，反向冲击通过了Pulsar附近，并将PWN推到一侧。
We report the results of X-ray (CXO) and radio (ATCA) observations of the pulsar wind nebula (PWN) powered by the young pulsar PSR J1016--5857, which we dub "the Goose" PWN. In both bands the images reveal a tail-like PWN morphology which can be attributed to pulsar's motion. By comparing archival and new CXO observations, we measure the pulsar's proper motion $μ=28.8\pm7.3$ mas/yr, yielding a projected pulsar velocity $v \approx 440\pm110$ km/s (at d=3.2 kpc); its direction is consistent with the PWN shape. Radio emission from the PWN is polarized, with the magnetic field oriented along the pulsar tail. The radio tail connects to a larger radio structure (not seen in X-rays) which we interpret as a relic PWN (also known as a plerion). The spectral analysis of the CXO data shows that the PWN spectrum softens from $Γ=1.7$ to $Γ\approx2.3-2.5$ with increasing distance from the pulsar. The softening can be attributed to rapid synchrotron burn-off, which would explain the lack of X-ray emission from the older relic PWN. In addition to non-thermal PWN emission, we detected thermal emission from a hot plasma which we attribute to the host SNR. The radio PWN morphology and the proper motion of the pulsar suggest that the reverse shock passed through the pulsar's vicinity and pushed the PWN to one side.
