Waves associated with interplanetary shocks driven by stream interactions

Details Waves associated with interplanetary shocks driven by stream interactions Waves associated with interplanetary shocks driven by stream interactions

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh42a..04b&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH42A-04

Physics

Plasma Physics

[7829] Space Plasma Physics / Kinetic Waves And Instabilities, [7851] Space Plasma Physics / Shock Waves, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

Interplanetary shocks can arise in the solar wind when a fast stream overtakes slow moving plasma. As they travel the shocks modify solar wind properties and also participate in the acceleration of solar energetic particles. The shocks are responsible for the generation of extended regions where low frequency waves are present. The extension and characteristics of the waves depend strongly on shock geometry and Mach number. When Mach number is low and the shock is quasi-perpendicular whistler waves remain close to the shock transition (both upstream and downstream). When the shock is quasi-parallel a large foreshock can form permeated by both, waves produced at the shock (whistler precursors), and waves that are generated upstream by backstreaming particles. Some of these upstream waves have frequencies f≈10-1 Hz, but others have irregular shapes and featureless spectra. During the years 2007-2009 corresponding to the solar minimum STEREO spacecraft have observed around 100 low Mach number (M 1.1~2.5) shocks. In this work we study the characteristics of the waves, and determine wave amplitude and the extension of the foreshocks as a function of θBn, and Mach number. The study of these waves is important because they participate in the acceleration of particles. We also study the role that waves can have in modifying shock structure. The fact that these shocks are weak makes them excellent candidates to gain insight into dissipation processes.

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