Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh51c1699c&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH51C-1699
Astronomy and Astrophysics
Astrophysics
[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7954] Space Weather / Magnetic Storms
Scientific paper
The erupting flux rope (EFR) model of CMEs (Chen 1996) has been shown to reproduce, to within 1-2% of the data, the observed dynamics of CMEs from the initial acceleration at the Sun and propagation to 1 AU based on STEREO data (Kunkel and Chen 2010; Chen and Kunkel 2010). Physically, it is shown that the heliospheric dynamics are determined by the competition of the Lorentz hoop force and the drag force. The best-fit solutions predict the footpoint separation distance Sf that is found to be consistent with the condidate source structures, produce temporal profiles of the poloidal flux injection function that coincide with those of the associated GOES SXR light curves, and for two CMEs observed STEREO, the best-fit solutions yield flux-rope magnetic fields with magnitudes in close agreement with those of the ejecta observed at 1 AU. The key factor in predicting the time of arrival at 1 AU and interpreting the observed in situ magnetic field profile is the 3D structure of the flux rope in relation to the observer at 1 AU. We extend the theory-model comparison analysis to include the 3D lux-rope geometry and calculate the detailed magnetic field profiles to be detected by the observing satellite at 1 AU. The technique is applied to a number of CMEs recently observed by SDO and STEREO focusing on events with data from the Sun to 1 AU, including in situ magnetic field and plasma data. We also include in our consideration the available magnetogram data, GOES SXR data, and EUV emissions associated with the CME events.
Chen Jiahua
Howard Russ A.
Kunkel Valbona
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