激波褶皱对微类星体内部激波模型的拯救：单尺度MHD视角
Shock corrugation to the rescue of the internal shock model in microquasars: The single-scale MHD view
AI总结：
针对微类星体喷流内部激波模型，本文利用单尺度MHD模拟研究初始非均匀等离子体壳层碰撞形成的褶皱激波，发现其可适度增强远下游辐射功率，并预测多波段偏振性质。
摘要：
尽管人们已进行大量尝试以限制模型的多样性，但关于天体物理喷流中能量耗散的问题至今仍未解决。一些最流行的模型假设，能量通过内部激波转移给粒子，而内部激波是喷流物质速度不均匀所导致的结果。在此背景下，我们研究碰撞等离子体壳层的结构与能量沉积，并将注意力集中于初始非均匀壳层的情形。这会导致畸变（褶皱）激波锋面的形成——近期已有研究表明，这种设置能够恢复相对论性磁化垂直激波中的粒子加速。我们的研究表明，与平面激波情形相比，非相对论性磁化垂直激波远下游区的辐射功率有适度增强。基于下游磁场的衰减率，我们对多波段偏振性质作出了预测。
英文摘要：
Questions regarding energy dissipation in astrophysical jets are open to date, despite of numerous attempts to limit the diversity of models. Some of the most popular models assume that energy is transferred to particles via internal shocks, which develop as a consequence of non-uniform velocity of the jet matter. In this context, we study the structure and energy deposition of colliding plasma shells, focusing our attention on the case of initially inhomogeneous shells. This leads to formation of distorted (corrugated) shock fronts -- a setup that has recently been shown to revive particle acceleration in relativistic magnetized perpendicular shocks. Our studies show that the radiative power of the far downstream of non-relativistic magnetized perpendicular shocks is moderately enhanced with respect to the flat shock cases. Based on the decay rate of downstream magnetic field, we make predictions for multiwavelength polarization properties.
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