Accelerated particles and hydromagnetic waves at co-rotating shocks

Details Accelerated particles and hydromagnetic waves at co-rotating shocks Accelerated particles and hydromagnetic waves at co-rotating shocks

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh41c..04s&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH41C-04

Physics

[2114] Interplanetary Physics / Energetic Particles, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2139] Interplanetary Physics / Interplanetary Shocks, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

Diffusive shock acceleration has dominated theories of shock acceleration of energetic particles for several decades including the origin of galactic cosmic rays in supernova shocks. Empirical studies of planetary bow shocks, especially the Earth’s, and shocks accompanying coronal mass ejections have produced useful comparisons with theory. However, many important quantitative questions remain such as the origin of the accelerated particles (their initial source and energy) and the efficiency with which they are accelerated. An essential feature of diffusive shock acceleration is the scattering of the particles back and forth across the shock by hydromagetic waves some of which are generated self-consistently by the accelerated particles moving upstream. A problem in studying the acceleration process is the large number of variables involved or potentially involved including the shock parameters (strength, speed, angle between the shock normal and the upstream magnetic field, θBN, supercriticality), the solar wind properties (density, temperature, anisotropy), the magnetic field(strength, power in turbulent fluctuations) and the energetic particles (intensity, energy spectrum, pitch angle distribution). An approach to this complexity is to sort a large number of cases by these various parameters so their effects might be isolated. This requirement is met by the large number of Forward and Reverse shocks that typically accompany Co-rotating Interaction Regions (CIRs) beyond about 2 AU. Fortunately, large numbers of such cases are present in Ulysses data at different radial distances where the spacecraft spent long time intervals at low latitudes. We have assembled a large data set of magnetic field, solar wind plasma and energetic particle measurements at CIR shocks and have begun analyzing them. One aspect of the study that is of interest to this session is the information contained about the more than three- dozen shocks that have been analyzed and that include a broad variety of types including a distribution that extends from parallel to perpendicular shocks.

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