Vortical field amplification and particle acceleration at rippled shocks

Abstract

Supernova Remnants (SNRs) shocks are believed to accelerate charged particles and to generate strong turbulence in the post-shock flow. From high-energy observations in the past decade, a magnetic field at SNR shocks largely exceeding the shock-compressed interstellar field has been inferred. We outline how such a field amplification results from a small-scale dynamo process downstream of the shock, providing an explicit expression for the turbulence back-reaction to the fluid whirling. The spatial scale of the $X-$ray rims and the short time-variability can be obtained by using reasonable parameters for the interstellar turbulence. We show that such a vortical field saturation is faster than the acceleration time of the synchrotron emitting energetic electrons.

4 pages, 3 figures; to appear in the proceedings of the RICAP-13, Roma International Conference on AstroParticle Physics

References in corpus (4)

• The Youngest Galactic Supernova Remnant: G1.9+0.3
• The contribution of star formation and merging to stellar mass buildup in galaxies
• Turbulent amplification of magnetic field driven by dynamo effect at rippled shocks
• Simulation of the growth of the 3D Rayleigh-Taylor instability in Supernova Remnants using an expanding reference frame

Cited by in corpus (5)

• Non-thermal emission from the reverse shock of the youngest galactic Supernova remnant G1.9+0.3
• Core-collapse supernovae in dense environments -- particle acceleration and non-thermal emission
• SNR G39.2-0.3, an Hadronic Cosmic Rays Accelerator
• Effect of acceleration and escape of energetic particles on spectral steepening at shocks
• Cross-field transport in Goldreich-Sridhar MHD turbulence