Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21a..02k&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SH21A-02
Physics
7513 Coronal Mass Ejections, 7531 Prominence Eruptions
Scientific paper
The density structure of a quiescent coronal flux rope is determined in terms of the specified magnetic field profile. We assume a uniform density and characteristic flow velocity at the photospheric foot points of a coronal flux rope and show that the density in the coronal portion of the flux rope is lowest on axis, where the field-lines are least twisted and the characteristic time-of-flight is briefest. Assuming that the structure of a coronal mass ejection (CME) corresponds to that of the pre-eruption flux rope, we find that these CMEs consist of somewhat-hollow magnetic flux ropes with foot points anchored in the photosphere. We have also tested our model CMEs against the data by computing synthetic coronagraph images. In cases where the CMEs parameters are consistent with both the analytical calculation and with prior modeling[1-4] of ``flux rope CME'' events, many characteristics of observed CME images are reproduced. [1] Chen, J. et al., 1997, ApJ, 490, L191 [2] Chen, J. et al., 2000, ApJ, 533, 481 [3] Krall, J. et al., 2000, ApJ, 539, 964 [4] Krall, J. et al., 2001, ApJ, 562, 1045 Supported by ONR.
Chen Jiahua
Krall Jonathan
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