A Density Model of Flux-Rope Coronal Mass Ejections

Details A Density Model of Flux-Rope Coronal Mass Ejections A Density Model of Flux-Rope Coronal Mass Ejections

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0478k&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0478

Physics

7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7531 Prominence Eruptions

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 depleted on axis, where the magnetic field lines are least twisted. Assuming that a flux-rope coronal mass ejection (CME) results from the eruption of a pre-existing coronal flux rope, the CME density is obtained.[1] The resulting model CME is tested against the data by computing synthetic coronagraph images.[2] In the case that these model CMEs are consistent with both the analytical calculation and with prior simulations of "flux rope CME" events[2,3] we find that many characteristics found in observed CME images are reproduced. This result explains the rim-cavity morphology often observed in CMEs. [1] Krall, J. and Chen, J., 2002, ApJ Lett, submitted [2] Chen, J. et al., 2000, ApJ, 533, 481 [3] Krall, J. et al., 2001, ApJ, 562, 1045 Supported by ONR and NASA.

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