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Cosmic ray transport and acceleration

机译：宇宙射线的传输与加速

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We review the theory of cosmic ray transport and acceleration with an emphasis on the underlying plasma physics and examine how that theory can be applied to sources such as supernova remnants and giant radio galaxies. Starting with Fermi's original model for scattering off moving magnetized clouds, we discuss quasilinear transport theory and its application to the acceleration of particles at shock fronts. We discuss problems of injection and the excitation of MHD turbulence by the accelerated particles. In the diffusive limit and at strong shocks this mechanism produces a differential energy spectrum of N(E) (proportional to E-2. Recent observations of supernova remnants suggest that their spectra may be steeper than this value. We discuss the transport and acceleration of energetic particles in highly correlated magnetic field structures. In this case particles have an enhanced probability of escape from the shock as they are trapped on field lines and the resulting spectrum is steepened up to a value of 2.5. Fast particle transport also seems to be required by observations of the structures of giant radio galaxy lobes as a function of frequency.
机译：我们回顾了宇宙射线传输和加速的理论，重点是基本的等离子体物理学，并研究了该理论如何应用于超新星遗迹和巨大的射电星系等来源。从费米最初的用于散射移动的磁化云的模型开始，我们讨论准线性传输理论及其在激波前沿的粒子加速中的应用。我们讨论了注入问题和由加速粒子激发的MHD湍流。在扩散极限和强烈冲击下，该机理产生了N（E）（与E-2成比例）的微分能谱。最近对超新星残余物的观察表明，它们的光谱可能比该值陡。高度相关的磁场结构中的高能粒子，在这种情况下，粒子被捕获在磁力线上的可能性更高，因为它们被捕获在磁力线上，因此产生的光谱陡峭到2.5，似乎还需要快速的粒子传输通过观察巨大的射电星系波瓣的结构作为频率的函数。

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