Magnetospheric ULF Oscillations Driven by Interior Kelvin-Helmholtz Modes

Details Magnetospheric ULF Oscillations Driven by Interior Kelvin-Helmholtz Modes Magnetospheric ULF Oscillations Driven by Interior Kelvin-Helmholtz Modes

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm33a1112c&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM33A-1112

Physics

2730 Magnetosphere: Inner, 2740 Magnetospheric Configuration And Dynamics, 7836 Mhd Waves And Instabilities (2149, 2752, 6050)

Scientific paper

Observations of field line resonances in the magnetosphere are characterized by a discrete set of ULF band frequencies. Determining the magnetospheric process that is responsible for this discrete set of frequencies has received much attention in the literature. The Kelvin-Helmholtz instability at the magnetopause boundary has been suggested as a possible candidate but it can only account for at most two discrete frequencies. Cavity mode oscillations have also been proposed but the geometric assumptions that must be made cannot account for the lowest frequency observations. In addition, cavity mode oscillations are seldom seen in magnetospheric observations. We present results from global magnetohydrodynamic (MHD) simulations of the solar wind/magnetosphere interaction that suggest the generation of interior Kelvin-Helmholtz (KH) modes inside the magnetosphere. These KH modes are generated locally, in the post dusk and pre dawn sectors of the magnetosphere. They arise as a result of counterstreaming sunward and tailward flows during periods of strong magnetospheric convection. We demonstrate how these interior KH modes can drive strong ULF oscillations inside the magnetosphere. A feature of these driven ULF oscillations is a discrete set of ULF band frequencies, a common feature of field line resonance observations.

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