Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53a..04k&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH53A-04
Physics
7513 Coronal Mass Ejections
Scientific paper
Observed flux-rope CME morphology depends on the underlying flux-rope geometry and its observed projection onto the two-dimensional plane of the sky. We use a simple parameterization of a three-dimensional flux rope to determine a "typical model flux-rope geometry" that corresponds to the "average observed flux-rope coronal mass ejection (CME) morphology" as observed at a leading-edge (LE) height of about 5 solar radii (e.g., LASCO/C2). The model flux rope, the curved axis of which is assumed to trace out an ellipse, can be described in terms of eccentricity of the ellipse, the width (minor diameter) of the flux rope at the apex, and the height of the apex above the solar surface. At an LE height of 5 solar radii, the resulting morphology is only a weak function of the foot point separation. Assuming that flux-rope expansion is self-similar, we have only two model-geometry parameters: the eccentricity and the aspect ratio (apex height over apex width). For each given pair of model parameters, we consider an ensemble of possible orientations (latitude, longitude, and rotation about the vertical direction) each with a corresponding synthetic coronagraph image. These images are used to produce statistical measures of the morphology for comparison to statistical measures of observed flux-rope CME morphology. The model parameters that best fit the observations constitute a prediction of the underlying geometry (eccentricity and aspect ratio) of a typical flux-rope CME. When STEREO confirms this prediction, the flux-rope hypothesis will be further validated. Supported by ONR and NASA
Chen Jiahua
Cyr Orville Chris St.
Krall Jonathan
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