Magnetic Flux Ropes from the Sun to 1 AU*

Details Magnetic Flux Ropes from the Sun to 1 AU* Magnetic Flux Ropes from the Sun to 1 AU*

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh22a..07k&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH22A-07

Physics

7513 Coronal Mass Ejections, 2111 Ejecta, Driver Gases, And Magnetic Clouds

Scientific paper

Any practical model of the dynamics of a coronal mass ejection (CME) and its interplanetary counterpart (ICME) must conform to available observational constraints from sun and to the earth; the upcoming STEREO mission will add significantly to those constraints. We present model/data comparisons for specific CME/ICME events near the sun (using coronagraph image data) and in the heliosphere (using in situ measurements) to show that the flux rope model of Chen and Krall[1-2] provides an accurate physics-based characterization of flux-rope CMEs over this range. We further show that quantitative results, such as the field energy required for eruption, depend on specific aspects of the flux rope geometry, such as the ratio (length/width) of the elliptical shape traced out by the flux-rope axis. It is this geometry that will be determined, for the first time, by STEREO. [1] Chen, J. 1996, JGR, 101, 27499 [2] Krall, J. et al., 2000, ApJ, 539, 964 *Work supported by ONR, NASA and NSF

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