标题： 从壳型超新星遗迹的无线电至伽马射线辐射：非线性激波加速模型的预测 显示英文标题

标题： Radio to Gamma-Ray Emission from Shell-type Supernova Remnants: Predictions from Non-linear Shock Acceleration Models

摘要： 超新星遗迹（SNRs）被广泛认为是银河宇宙射线的主要来源。 这些高能粒子可以通过与周围等离子体的相互作用产生伽马射线和较低能量的光子。 在本文中，我们展示了壳层状SNRs中非线性激波结构和加速过程以及光子发射的蒙特卡罗模拟结果。 这些非线性是加速宇宙射线对受激等离子体的动力学影响的副产品，并导致宇宙射线的分布偏离纯幂律。 这种偏差对于加速效率和光谱考虑至关重要，产生了与测试粒子预测显著不同的GeV/TeV强度比。 使用SNR扩展的Sedov标度解来估算重要的激波参数，以输入到蒙特卡罗模拟中。 我们计算了产生中性π介子衰变、制动辐射、逆康普顿和同步辐射的离子和电子分布，从而从射频频率到伽马射线能量产生完整的光子谱。 由于在中等密度星际区域中膨胀的SNR壳层的空间和时间限制导致加速停止，可能在TeV能量范围内产生光谱截止；这些与Whipple对未识别的EGRET源的TeV上限一致。 低密度环境中的超新星遗迹产生更高能量的宇宙射线，在亚TeV能量下主要产生逆康普顿辐射；这样的源在GeV能量下通常会是伽马射线暗弱的。 显示英文摘要

摘要： Supernova remnants (SNRs) are widely believed to be the principal source of galactic cosmic rays. Such energetic particles can produce gamma-rays and lower energy photons via interactions with the ambient plasma. In this paper, we present results from a Monte Carlo simulation of non-linear shock structure and acceleration coupled with photon emission in shell-like SNRs. These non-linearities are a by-product of the dynamical influence of the accelerated cosmic rays on the shocked plasma and result in distributions of cosmic rays which deviate from pure power-laws. Such deviations are crucial to acceleration efficiency and spectral considerations, producing GeV/TeV intensity ratios that are quite different from test particle predictions. The Sedov scaling solution for SNR expansions is used to estimate important shock parameters for input into the Monte Carlo simulation. We calculate ion and electron distributions that spawn neutral pion decay, bremsstrahlung, inverse Compton, and synchrotron emission, yielding complete photon spectra from radio frequencies to gamma-ray energies. The cessation of acceleration caused by the spatial and temporal limitations of the expanding SNR shell in moderately dense interstellar regions can yield spectral cutoffs in the TeV energy range; these are consistent with Whipple's TeV upper limits on unidentified EGRET sources. Supernova remnants in lower density environments generate higher energy cosmic rays that produce predominantly inverse Compton emission at super-TeV energies; such sources will generally be gamma-ray dim at GeV energies.