论文标题
年轻的Magnetar Swift J1818.0-1607的第一次爆发的深X射线和无线电观察
Deep X-ray and radio observations of the first outburst of the young magnetar Swift J1818.0-1607
论文作者
论文摘要
Swift J1818.0-1607是一种无线电大通磁铁，自旋周期为1.36 s，B〜3E14 g的偶极磁场强度与银河脉冲星人群相比非常年轻。我们在此处报告了使用XMM-Newton，Nustar和Swift从2020年3月至2021年10月的第一次爆发以及其硬X射线排放的整体上限，并在此报告了这款年轻磁铁的长期X射线监测活动。 1-10 KEV磁盘光谱是通过吸收的黑体（温度为kt_bb〜1.1 keV）很好地建模的，并且发射区域的半径明显从〜0.6至〜0.2 km降低。我们还确认围绕〜50'''和〜110''的源周围的明亮弥漫性X射线发射。定时分析显示出较大的扭矩变异性，平均旋转速率nudot〜-2.3e-11 Hz^2，随着时间的流逝，大小似乎会降低。 We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse radio emission located at ~90'' to the west of磁铁。我们暂时建议弥漫性X射线发射是由于粉尘散射的光环造成的，并且射电结构可能与该年轻脉冲星的超新星残留物相关，它基于其形态。
Swift J1818.0-1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B~3E14 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in March 2020 until October 2021, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT_BB~1.1 keV, and apparent reduction in the radius of the emitting region from ~0.6 to ~0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ~50'' and ~110''. A timing analysis revealed large torque variability, with an average spin-down rate nudot~-2.3E-11 Hz^2 that appears to decrease in magnitude over time. We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse radio emission located at ~90'' to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology.
