A Physical Description of Coronal Pulse Wave Dynamics

Details A Physical Description of Coronal Pulse Wave Dynamics A Physical Description of Coronal Pulse Wave Dynamics

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp21b..10w&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP21B-10

Physics

7509 Corona

Scientific paper

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.

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