论文标题
碰撞流中的粒子加速度：二进制恒星风和其他双震结构
Particle Acceleration in Colliding Flows: Binary Star Winds and Other Double-Shock Structures
论文作者
论文摘要
垂直于环境磁场传播的冲击波会加速颗粒的速度要比平行传播方案快得多。但是，垂直加速度在冲击过度的圆形粒子轨道过度之后停止。同时，它可能会因一对垂直冲击而绑定的超人碰撞等离子体导致的流量继续。尽管我们详细考虑的双震加速度机制对于热颗粒没有优势，但预启动的颗粒可能避免加速的过早末端。我们认为，如果它们的吉拉迪乌斯超过了冲击之间的主要湍流量表，那么这些颗粒可能会反复穿越互换空间，然后再被震惊的血浆带走。此外，输入类似速度的冲击之间的空间$ u_ {1} \ of u_ {2} \ of C $，此类粒子开始以固定角度$ \ 35.3^{\ circ} $在冲击表面上以固定角度$ \ 35.3^{\ circ}弹跳。 Their drift along the shock fronts is slow, $V_{d}\sim\left|u_{2}-u_{1}\right|\ll c$, so that it will take $N\sim Lc/\left|u_{2}-u_{1}\right|d\gg1$ bounces before they escape the accelerator (here, $L$ is the size of the shocks $ d $是它们之间的差距）。由于这些颗粒每个周期的能量超过十倍（连续两次弹跳），因此我们调用可能限制加速度的其他可能损失。它们包括由于波纹冲击而导致的漂移，上游磁场的非平行相互取向以及辐射损失。
A shock wave propagating perpendicularly to an ambient magnetic field accelerates particles considerably faster than in the parallel propagation regime. However, the perpendicular acceleration stops after the shock overruns a circular particle orbit. At the same time, it may continue in flows resulting from supersonically colliding plasmas bound by a pair of perpendicular shocks. Although the double-shock acceleration mechanism, which we consider in detail, is not advantageous for thermal particles, pre-energized particles may avoid the premature end of acceleration. We argue that if their gyroradius exceeds the dominant turbulence scale between the shocks, these particles might traverse the intershock space repeatedly before being carried away by the shocked plasma. Moreover, entering the space between the shocks of similar velocities $u_{1}\approx u_{2}\approx c$, such particles start bouncing between the shocks at a fixed angle $\approx 35.3^{\circ}$ to the shock surface. Their drift along the shock fronts is slow, $V_{d}\sim\left|u_{2}-u_{1}\right|\ll c$, so that it will take $N\sim Lc/\left|u_{2}-u_{1}\right|d\gg1$ bounces before they escape the accelerator (here, $L$ is the size of the shocks and $d$ is the gap between them). Since these particles more than ten-fold their energy per cycle (two consecutive bounces), we invoke other possible losses that can limit the acceleration. They include drifts due to rippled shocks, the nonparallel mutual orientation of the upstream magnetic fields, and radiative losses.
