Magnetic Geometry of Accelerating CMEs

Details Magnetic Geometry of Accelerating CMEs Magnetic Geometry of Accelerating CMEs

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh22a..08c&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH22A-08

Physics

7513 Coronal Mass Ejections

Scientific paper

It has been known that the main acceleration phase of a coronal mass ejection (CME) is localized to within 3--4 Rs of the Sun. Recently, it has been theoretically shown [1] that if the initial structure is a magnetic flux rope, the main acceleration peaks at apex height Z* ≈ Sf/2, where Sf is the separation distance between the two footpoints anchored in the photosphere. This scaling property is therefore an observational signature of the magnetic geometry. The Sf-scaling law is universal in that it only depends on the pre-eruptive flux-rope geometry in 3-D. The initial comparisons with representative LASCO CMEs (C1-C2-C3 data) showed that this prediction is consistent with observations [1]. We will present further model-data comparisons using the archived LASCO data as well as eruptive prominence data. We discuss the significant improvement in theory-data comparison that will be possible with the expected STEREO data. Particularly, the two observing perspectives will allow one to better constrain the flux-rope geometry during the main acceleration phase, especially with respect to the footpoint separation Sf. In addition, the near-Sun observing capabilities (down to ˜0.5 Rs) and high cadence of COR1 will provide much better resolved observations of the initial acceleration of CMEs. 1.~Chen, J., and J. Krall, JGR, 108, 1410, doi:10.1029/2003JA009849, 2003. Work supported by ONR and NASA

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