Injection to rapid diffusive shock acceleration at perpendicular shocks in partially ionized plasmas

Abstract

We present a three-dimensional hybrid simulation of a collisionless perpendicular shock in a partially ionized plasma for the first time. In this simulation, the shock velocity and the upstream ionization fraction are Vsh ~ 1333 km/s and fi ~ 0.5, that are typical values for isolated young supernova remnants in the interstellar medium. We confirm previous two-dimensional simulation results that downstream hydrogen atoms leak into the upstream region, they are accelerated by the pickup process in the upstream region, and large magnetic field fluctuations are generated both in the upstream and downstream regions. In addition, we find that the magnetic field fluctuations have three-dimensional structures and the leaking hydrogen atoms are injected to the diffusive shock acceleration at the perpendicular shock after the pickup process. The observed diffusive shock acceleration can be interpreted as the shock drift acceleration with scattering. Particles are accelerated to v ~ 100 Vsh ~ 0.3c within ~ 100 gyroperiods in this simulation. The acceleration time scale is faster than that of the diffusive shock acceleration in parallel shocks. Our simulation results suggest that supernova remnants can accelerate cosmic rays to 10^{15.5} eV (the knee) during the Sedov phase.

7 pages, 7 figures, accepted for publication in ApJ

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• Magnetic field generation by an inhomogeneous return current
• Fast Particle Acceleration at Perpendicular Shocks with Uniform Upstream Magnetic Field and Strong Downstream Turbulence
• Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
• Diffusive shock acceleration at oblique high Mach number shocks
• Particle acceleration in a shock wave propagating to an inhomogeneous medium
• Polarized Balmer Line Emission from Supernova Remnant Shock Waves Efficiently Accelerating Cosmic Rays
• X-ray Line Diagnostics of Ion Temperature at Cosmic-Ray Accelerating Collisionless Shocks
• Radiative transfer of hydrogen lines from supernova remnant shock waves: contributions of 2s-state hydrogen atoms
• Particle acceleration and magnetic field amplification by relativistic shocks in inhomogeneous media
• Escape of cosmic rays from perpendicular shocks in the circumstellar magnetic field
• Reinterpretation of the Fermi acceleration of cosmic rays in terms of the ballistic surfing acceleration in supernova shocks
• Property of downstream turbulence driven by the special relativistic shock-clump interaction
• Escape of cosmic rays from perpendicular shocks in the interstellar magnetic field
• Magnetic field generation by charge exchange in a supernova remnant in the early universe