Lower-hybrid Wave Heating of Electrons in the Cosmic Ray Precursor of Collisionless Shocks

Details Lower-hybrid Wave Heating of Electrons in the Cosmic Ray Precursor of Collisionless Shocks Lower-hybrid Wave Heating of Electrons in the Cosmic Ray Precursor of Collisionless Shocks

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.3111r&link_type=abstract

American Astronomical Society, HEAD meeting #10, #31.11

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The mechanism for heating electrons at collisionless shock waves has been the subject of both theoretical and observational study for many years. In Ghavamian et al 2007, we presented observational evidence for an inverse square relation between the electron-to-proton temperature ratio and the shock speed at the outer blast wave of supernova remnants. In that paper we discussed how lower-hybrid waves generated in the cosmic-ray precursor could explain such a relationship by heating the electrons to a common temperature independent of both shock speed and the strength of the ambient magnetic field. In this talk, we review that work and explore the mechanism of lower-hybrid wave heating in more depth. Specifically we examine the growth rate of lower-hybrid waves under both kinetic (resonant) and reactive (non-resonant) cases and compare it to the rate at which electrons could damp the instability. Only the kinetic case is found to be subject to instability. We discuss lower-hybrid waves in the context of other instabilities in the cosmic-ray precursor including the magnetic field amplification by modified Alfv\'{e}n waves, previously predicted by Bell and coworkers.

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