Kelvin-Helmholtz Instability and Turbulence Forming Behind a CME-driven Shock.

Details Kelvin-Helmholtz Instability and Turbulence Forming Behind a CME-driven Shock. Kelvin-Helmholtz Instability and Turbulence Forming Behind a CME-driven Shock.

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh53a1245m&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH53A-1245

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7845 Particle Acceleration, 7851 Shock Waves (4455)

Scientific paper

We have found that a fast CME propagating through a bimodal solar wind produces variety of unexpected results. By means of a three-dimensional (3-D) numerical ideal magnetohydrodynamics (MHD) model we explore the interaction of a fast CME with a solar wind that possesses fast and slow speed solar wind at high and low latitude respectively. Within this model system, a CME erupts from the coronal streamer belt with an initial speed in excess of 1000 km/s which naturally drives a forward shock. An indentation in the shock forms at low latitude where it propagates through the slow solar wind. This indentation causes the fast-mode shock to deflect the flow toward the impinging flux rope. The plasma flow then must reverses direction to move around the rope, resulting in strong velocity shears. The shear flow is shown to be susceptible to the Kelvin-Helmholtz instability, which results in significant turbulence producing an environment very conducive to particle acceleration.

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