HR: 0830h
AN: SP21B-10    [Abstracts]
TI: A Physical Description of Coronal Pulse Wave Dynamics
AU: * Wills-Davey, M J
EM: meredith@boulder.swri.edu
AF: Southwest Reserach Institute, 1050 Walnut St., Suite 400, Boulder, CO 80302 United States
AB: Many of the studies concerning coronal pulse waves (also called "EIT waves") have interpreted these phenomena as fast-mode magnetoacoustic wave fronts. In many respects, this explanation has proved inconsistent with observations. Recently, it has been postulated that coronal pulse waves are actually non-linear MHD solitons. However, one characteristic of the soliton solution has proved problematic: a simple analytic consideration requires that solitons travel at velocities much faster than those observed in coronal pulse waves. We demonstrate that a slow MHD soliton solution is possible; however, the stability of this solution requires very specific MHD geometry. Fortunately, this geometry happens to be consistent with the conditions that support coronal pulse waves.
DE: 7509 Corona
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly