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

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dppbp1022k&link_type=abstract

American Physical Society, 46th Annual Meeting of the Division of Plasma Physics, 15-19 November, 2004, Savannah, GA. MEETING I

Physics

Plasma Physics

Scientific paper

Any practical model of the dynamics of a coronal mass ejection (CME) must conform to available observational constraints from sun and to the earth. We present model/data comparisons near the sun (using coronagraph image data) and in the heliosphere (using in situ measurements) to show that our flux rope model[1-3] provides an accurate physics-based characterization of flux-rope coronal mass ejections over this range. As our understanding increases, we are approaching a point where we can use near-sun data to provide model inputs, with the model output being a prediction of near-earth magnetic fields. These magnetic fields can drive geomagnetic storms, an element of our local ``space weather''. [1] Chen, J. 1996, JGR, 101, 27499 [2] Krall, J. et al., 2000, ApJ, 539, 964 [3] Chen, J., and Krall, J. 2003, JGR, 108, 1410

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