Understanding the response of the magnetosphere to modest, moderate, and strong solar wind IMF driving

Details Understanding the response of the magnetosphere to modest, moderate, and strong solar wind IMF driving Understanding the response of the magnetosphere to modest, moderate, and strong solar wind IMF driving

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsm42a..06g&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM42A-06

Physics

2700 Magnetospheric Physics (6939), 2753 Numerical Modeling, 2788 Magnetic Storms And Substorms (7954)

Scientific paper

Our understanding of how the magnetosphere dissipates the energy acquired during periods of southward IMF is well developed in the limits of modest (substorms) and strong driving (storms). However the response of the magnetosphere to extended periods of moderately southward IMF remains unclear. For this moderate level of driving, the magnetosphere can exhibit either steady magnetospheric convection (SMC), in which a steady state balance of energy inflow and dissipation appears to be attained, or Sawtooth behavior, in which there are periodic injections of energetic particles into the inner magnetosphere. While we have identified these apparently different modes of the magnetosphere in individual events, we have yet to understand the differences in magnetospheric response responsible for them; i.e., are Sawtooth events periodic substorms, are they and/or SMCs related to storm conditions, in which they are often observed. We will explore the similarities and differences of storm, SMC, and sawtooth behavior through global MHD simulations of 4 specific events. The first is the Halloween storm (Oct 29-30) of 2002, during which we will focus particularly on the apparent Sawtooth activity late on Oct 29. The second is the February 3, 1998 SMC event studied by the NSF GEM program. The third event is the well known Sawtooth period of April 18, 2002. The final event is the isolated substorm of August 11, 2002. This presentation will provide an overview of the simulation results and explore the differences in magnetospheric configuration and evolution for these events.

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