On the Structure and Scale of Cosmic Ray Modified Shocks

M. A. Malkov; P. H. Diamond; R. Z. Sagdeev

doi:10.1088/0741-3335/52/12/124006

paper

On the Structure and Scale of Cosmic Ray Modified Shocks

arXiv:1007.3042 · doi:10.1088/0741-3335/52/12/124006

Abstract

Strong astrophysical shocks, diffusively accelerating cosmic rays (CR) ought to develop CR precursors. The length of such precursor $L_{p}$ is believed to be set by the ratio of the CR mean free path $λ$ to the shock speed, i.e., $L_{p} \sim c λ / V_{s h} \sim c r_{g} / V_{s h}$ , which is formally independent of the CR pressure $P_{c}$ . However, the X-ray observations of supernova remnant shocks suggest that the precursor scale may be significantly shorter than $L_{p}$ which would question the above estimate unless the magnetic field is strongly amplified and the gyroradius $r_{g}$ is strongly reduced over a short (unresolved) spatial scale. We argue that while the CR pressure builds up ahead of the shock, the acceleration enters into a strongly nonlinear phase in which an acoustic instability, driven by the CR pressure gradient, dominates other instabilities (at least in the case of low $β$ plasma). In this regime the precursor steepens into a strongly nonlinear front whose size scales with \emph{the CR pressure}as $L_{f} \sim L_{p} \cdot (L_{s} / L_{p})^{2} (P_{c} / P_{g})^{2}$ , where $L_{s}$ is the scale of the developed acoustic turbulence, and $P_{c} / P_{g}$ is the ratio of CR to gas pressure. Since $L_{s} ≪ L_{p}$ , the precursor scale reduction may be strong in the case of even a moderate gas heating by the CRs through the acoustic and (possibly also) the other instabilities driven by the CRs.

EPS 2010 paper, to appear in PPCF

On the Structure and Scale of Cosmic Ray Modified Shocks

Abstract

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