从超新星遗迹的流体动力学模拟计算同步辐射和逆康普顿辐射的方法
A method for computing synchrotron and inverse-Compton emission from hydrodynamic simulations of supernova remnants
摘要：
超新星遗迹（SNRs）的观测特征是非常复杂的，在其几何形状和光谱特性方面，主要是由非热同步辐射和逆康普顿散射。提出了一种基于三维流体动力学模拟的宽带信噪比后处理方法。从流体动力学的数据，我们估计的非热电子的分布加速在冲击波，并遵循随后的演变，因为它们失去或获得能量的绝热膨胀或压缩和辐射发射能量。作为第一个测试案例，我们使用一个双极超新星膨胀到多云介质的模拟。我们发现，我们的方法定性地再现了典型信噪比的主要观测特征，并产生与观测结果一致的通量。从而允许在更多扩展的模型组中进一步使用。
英文摘要：
The observational signature of supernova remnants (SNRs) is very complex, in terms of both their geometrical shape and their spectral properties, dominated by non-thermal synchrotron and inverse-Compton scattering. We propose a post-processing method to analyse the broad-band emission of SNRs based on three-dimensional hydrodynamical simulations. From the hydrodynamical data, we estimate the distribution of non-thermal electrons accelerated at the shock wave and follow the subsequent evolution as they lose or gain energy by adiabatic expansion or compression and emit energy by radiation. As a first test case, we use a simulation of a bipolar supernova expanding into a cloudy medium. We find that our method qualitatively reproduces the main observational features of typical SNRs and produces fluxes that agree with observations to within a factor of a few. allowing for further use in more extended sets of models.
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