Wave generation and magnetic field amplification in astrophysical shocks

Details Wave generation and magnetic field amplification in astrophysical shocks Wave generation and magnetic field amplification in astrophysical shocks

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aps..dppyp6051g&link_type=abstract

American Physical Society, 50th Annual Meeting of the Division of Plasma Physics, November 17-21, 2008, abstract #YP6.051

Physics

Plasma Physics

Scientific paper

Supernovae remnant shocks, producing Cosmic Rays (CR), and coronal mass ejection shocks, producing Solar Energetic Particles (SEP), have different features, but in both scenarios waves are known to propagate and to amplify the magnetic field and turbulence in the upstream region of the shocks. We analyze Bell's instability [1], in which small-scale non-resonant wave modes are driven by cosmic ray ions streaming in the shock precursor along a background magnetic field B0, and driving a current. We use hybrid simulations to study the feedback of magnetic turbulence produced on cosmic ray trajectories; our results show a significant magnetic field enhancement, strongly dependent on the relative flow velocity of the ion species, and show the formation of plasma-depleted cavities. We find that the saturation of the instability is associated with the sustainability of the current. The non-linear growth phase and the saturation phase are explored in detail, and a discussion of the relevance of the mechanism to the CR and SEP scenarios is also presented. [1] A. R. Bell, Mon. Not. R. Astron. Soc. 353, 550, 2004

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