论文标题
Supernova Remnant RX J1713.7 $ - $ 3946的西北壳的X射线热点
X-ray Hotspots in the Northwest Shell of the Supernova Remnant RX J1713.7$-$3946
论文作者
论文摘要
Supernova Remnant（SNR）RX J1713.7 $ - $ 3946是宇宙射线的最佳加速器之一，因为它具有强大的非热X射线射线和伽马射线辐射。我们已经分析了RX J1713.7 $ -3946的西北边缘的累积\ Chandra \观测值，总曝光时间为$ \ sim $ 266 ks。我们检测到大量类似点的来源，称为``热点''，它们可能与残留物相关。热点的光谱由吸收的幂律模型很好地描述。 The spectral properties ($10^{21}\ \mathrm{cm^{-2}}\lesssim N_H \lesssim 10^{23}\ \mathrm{cm^{-2}}$ and $ 0.5\lesssim Γ\lesssim 6$) are different from diffuse X-ray emission in RX j1713.7 $ - $ 3946，较难的热点往往具有较大的$ n_h $。我们还确认某些热点的每年和每月通量变化。我们建议RX J1713.7 $ - $ 3946嵌入在复杂的环境中，在复杂的环境中，某些密集的分子团块和核心存在于风吹式腔内，而热点痕迹会导致SNR和密集的分子芯的相互作用引起的同步，并具有$ 10^^^^5^^5}^^5}^^5}^^5} \ mathrm {cm}^{ - 3} $。热点的X射线辐射可能是从与加速质子与核心相互作用产生的电击和次级电子加速的主要电子中发出的。
The supernova remnant (SNR) RX J1713.7$-$3946 is one of the best-studied accelerators of cosmic rays because of its strong nonthermal X-ray and gamma-ray radiation. We have analyzed accumulated \chandra\ observations with a total exposure time of $\sim$266 ks in the northwest rim of RX J1713.7$-$3946. We detect a substantially large number of point-like sources, referred to as ``hotspots'', which are likely associated with the remnant. The spectra of the hotspots are well described by an absorbed power-law model. The spectral properties ($10^{21}\ \mathrm{cm^{-2}}\lesssim N_H \lesssim 10^{23}\ \mathrm{cm^{-2}}$ and $ 0.5\lesssim Γ\lesssim 6$) are different from diffuse X-ray emission in RX J1713.7$-$3946, and the harder hotspot tends to have the larger $N_H$. We also confirm yearly and monthly variabilities of flux for some hotspots. We propose that RX J1713.7$-$3946 is embedded in a complex surroundings where some dense molecular clumps and cores exist inside a wind-blown cavity, and that the hotspot traces synchrotron emission caused by an interaction of shock waves of the SNR and dense molecular cores with a number density of $10^{5}-10^{7}~ \mathrm{cm}^{-3}$. The X-ray radiation of the hotspot might be emitted from both primary electrons accelerated at the shocks and secondary electrons produced by the interaction of accelerated protons with the cores.
