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Session 1 - Chromosphere, Corona, Flares.
Display session, Friday, June 27
Ballroom B, Chair: Charles Kankelborg

[1.10] Fitting a 3-d analytic model of the Coronal Mass Ejection to observations

S. Gibson (NASA/GSFC NRC), R. Fisher (NASA/GSFC), R. Howard (NRL), B. Thompson (NASA/GSFC ARC)

We present the application of an analytic magnetohydrodynamic model (Gibson and Low, 1997) to observations of the time-dependent expulsion of three-dimensional Coronal Mass Ejections (CMEs) out of the solar corona. The model relates the white-light appearance of the CME to its internal magnetic field, which takes the form of a closed bubble, filled with a partly anchored, twisted magnetic flux rope and embedded in an otherwise open background field. The density distribution frozen into the expanding CME magnetic field is fully three-dimensional, and can be integrated along the line of sight to reproduce observations of scattered white light. The model is able to reproduce the conspicuous three features often associated with CMEs as observed with white-light coronagraphs: a surrounding high-density region, an internal low-density cavity, and a high-density core. By varying the model parameters, including the location and orientation of the CME magnetic axis relative to the limb, we are able to fit the model directly to examples of CMEs observed by the HAO/SMM Coronagraph, the HAO/Mark III K-Coronameter, and also to an event observed both by the SOHO/LASCO coronagraphs and the SOHO/EIT EUV coronal imager.


The author(s) of this abstract have provided an email address for comments about the abstract: gibson@serts.gsfc.nasa.gov

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