超新星遗迹RX J0852-4622西北缘的非热辐射性质
Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852-4622
摘要：
超新星遗迹（SNR）RX J 0852 -4622（Vela Jr.，G266.6-1.2）是研究多TeV粒子加速和银河系宇宙射线起源的最重要的信噪比之一，因为它具有很强的同步辐射X射线和TeV γ射线辐射，它们都表现出类似于壳的形貌。使用XMM-牛顿档案数据组成的多个指向观测的西北边缘的残余，我们调查的非热X射线发射的空间特性作为一个函数的距离从外部冲击波。所有的X射线光谱都很好地再现了吸收的幂律模型高于2千电子伏。结果发现，光谱表现出逐渐软化，从边缘区域的光子指数2.56到内部区域的2.96。我们表明，这种径向配置文件可以解释为一个逐渐减少的截止能量的电子光谱由于同步辐射冷却。通过使用一个简单的光谱演化模型，包括连续的同步辐射损失，光谱软化可以再现与磁场强度在激波后流小于几十μ G。如果这是SNR壳层中的典型磁场，则伽马射线发射将通过高能电子的逆康普顿散射来解释，该逆康普顿散射也产生同步加速器X射线发射。Nustar和ASTRO-H的未来硬X射线成像观测和切伦科夫望远镜阵列（CTA）的TeV伽马射线观测将使我们能够探索X射线光谱系统软化的其他可能解释。
英文摘要：
The supernova remnant (SNR) RX J0852-4622 (Vela Jr., G266.6-1.2) is one of the most important SNRs for investigating the acceleration of multi-TeV particles and the origin of Galactic cosmic rays because of its strong synchrotron X-ray and TeV gamma-ray emission, which show a shell-like morphology similar to each other. Using the XMM-Newton archival data consisting of multiple pointing observations of the northwestern rim of the remnant, we investigate the spatial properties of the nonthermal X-ray emission as a function of distance from an outer shock wave. All X-ray spectra are well reproduced by an absorbed power-law model above 2 keV. It is found that the spectra show gradual softening from a photon index 2.56 in the rim region to 2.96 in the interior region. We show that this radial profile can be interpreted as a gradual decrease of the cutoff energy of the electron spectrum due to synchrotron cooling. By using a simple spectral evolution model that includes continuous synchrotron losses, the spectral softening can be reproduced with the magnetic field strength in the post-shock flow to less than several tens of uG. If this is a typical magnetic field in the SNR shell, gamma-ray emission would be accounted for by inverse Compton scattering of high-energy electrons that also produce the synchrotron X-ray emission. Future hard X-ray imaging observations with Nustar and ASTRO-H and TeV gamma-ray observations with the Cherenkov Telescope Array (CTA) will allow to us to explore other possible explanations of the systematic softening of the X-ray spectra.
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