Astronomy and Astrophysics – Astronomy
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0514k&link_type=abstract
American Astronomical Society, SPD meeting #34, #05.14; Bulletin of the American Astronomical Society, Vol. 35, p.816
Astronomy and Astrophysics
Astronomy
Scientific paper
A density model is developed for a coronal flux rope with a specified magnetic field configuration. We find that the flux-rope plasma density is enhanced off axis, where the magnetic field lines are least twisted. This occurs as a result of the flow of plasma from the foot points to the apex of the flux rope. The center-to-edge density enhancement is sensitive to the current profile within the flux rope, with a more highly-peaked channel resulting in a greater center-to-edge density enhancement. Assuming self-similar expansion of the flux rope cross section from foot points (flux rope radius af) to the corona (radius a), the maximum possible density enhancement is ρ (r=a)/ρ (r=0) ˜= a/af. Assuming that a flux-rope coronal mass ejection (CME) results from the eruption of a coronal flux rope, the CME density, neglecting the prominence, is obtained. The resulting model CME is tested against the data by computing synthetic coronagraph images. Thus, the observed rim-cavity morphology of CMEs is explained.
Work supported by ONR and NASA
Chen Jiahua
Krall Jonathan
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