论文标题
PSR J1709-4429的适当运动及其与SNR G343.1-2.3的关系
PSR J1709-4429's Proper Motion and its Relationship to SNR G343.1-2.3
论文作者
论文摘要
我们在2018 - 2019年期间在4个时代中获得了PSR J1709-4429的显着脉冲星云（PWN）的670 KS CXO ACI图像。与档案2004数据集的比较，在86 \ pm 9度（1 Sigma组合统计和系统的不确定性）的PA上提供了PULSAR正确运动MU = 13 \ pm 3 mas/yr，排除了SNR G343.1-2.3中心附近的出生。在Pulsar的特征年龄17 kyr时，可以通过祖细胞风，出生踢和PWN流出的结合来保留该关联。但是，相关的TEV发射可能表明早期的超新星爆炸。 X射线图像的期间比较表明PWN是动态的，但是我们无法从BLOB运动中最终测量流速。 Pulsar产生了无线电/X射线风泡，我们认为PWN的长狭窄喷气机被震惊的脉冲星风扫回了该空腔。这些喷气机可以追踪PWN流的极性磁场线，这是数值建模的有趣挑战。
We have obtained a deep 670 ks CXO ACIS image of the remarkable pulsar wind nebula (PWN) of PSR J1709-4429, in 4 epochs during 2018-2019. Comparison with an archival 2004 data set provides a pulsar proper motion mu = 13 \pm 3 mas/yr at a PA of 86 \pm 9 degree (1 sigma combined statistical and systematic uncertainties), precluding birth near the center of SNR G343.1-2.3. At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick and PWN outflow. Associated TeV emission may, however, indicate explosion in an earlier supernova. Inter-epoch comparison of the X-ray images shows that the PWN is dynamic, but we are unable to conclusively measure flow speeds from blob motion. The pulsar has generated a radio/X-ray wind bubble, and we argue that the PWN's long narrow jets are swept back by shocked pulsar wind venting from this cavity. These jets may trace the polar magnetic field lines of the PWN flow, an interesting challenge for numerical modeling.
