Particle Acceleration in Colliding Flows: Binary Star Winds and Other Double-Shock Structures

Mikhail Malkov; Martin Lemoine

doi:10.1103/PhysRevE.107.025201

paper

Particle Acceleration in Colliding Flows: Binary Star Winds and Other Double-Shock Structures

arXiv:2212.08788 · doi:10.1103/PhysRevE.107.025201

Abstract

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, $V_{d} \sim ∣ u_{2} - u_{1} ∣ ≪ c$ , so that it will take $N \sim L c / ∣ u_{2} - u_{1} ∣ d ≫ 1$ 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.

21 pages, 13 figure, improved in V.2

Particle Acceleration in Colliding Flows: Binary Star Winds and Other Double-Shock Structures

Abstract

References in corpus (12)