Three-Dimensional Simulation of Kelvin-Helmholtz Modes at the Magnetospheric Boundary

Details Three-Dimensional Simulation of Kelvin-Helmholtz Modes at the Magnetospheric Boundary Three-Dimensional Simulation of Kelvin-Helmholtz Modes at the Magnetospheric Boundary

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm53a..02o&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SM53A-02

Physics

2723 Magnetic Reconnection (7526, 7835), 2724 Magnetopause And Boundary Layers, 2748 Magnetotail Boundary Layers, 2752 Mhd Waves And Instabilities (2149, 6050, 7836), 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

The physics of the magnetospheric boundaries is central to the transport of mass, energy, and momentum into magnetosphere. Here much attention has been given to magnetic reconnection. However, in recent years Kelvin Helmholtz (KH) modes have become an increasing focus for the interaction between the magnetosphere and the solar wind. Recent results indicate that three-dimensional aspects are of crucial importance for this interaction. KH modes are able to trigger reconnection as a secondary process even in cases where the IMF and the magnetospheric field are largely aligned. The mode of reconnection, however, is very different in two dimensions compared to three dimensions. We will review the relevant recent results from these studies and present new results for this process. Particularly, we will address the questions of the quantitative mass transport associated with three-dimensional KH modes as a function of IMF orientation. The presentation also address the issue of the plasma transport further into the magnetosphere.

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