HR: 11:50h
AN: SH22A-07    [Abstracts]
TI: Magnetic Flux Ropes from the Sun to 1 AU*
AU: * Krall, J
EM: krall@ppdmail.nrl.navy.mil
AF: Plasma Physics Division, Naval Research Laboratory, Code 6790, Washington, DC 20375-5000 United States
AU: Yurchyshyn, V B
EM: vayur@bbso.njit.edu
AF: Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314 United States
AU: St. Cyr, O C
EM: Chris.StCyr@nasa.gov
AF: Solar Physics Branch, NASA-Goddard Space Flight Center, Code 682, Greenbelt, MD 20771 United States
AU: St. Cyr, O C
EM: Chris.StCyr@nasa.gov
AF: Department of Physics, The Catholic University of America, 620 Michigan Ave., N.E., Washington, DC 20064 United States
AU: Chen, J
EM: chen@ppdmail.nrl.navy.mil
AF: Plasma Physics Division, Naval Research Laboratory, Code 6790, Washington, DC 20375-5000 United States
AB: 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
DE: 7513 Coronal mass ejections
DE: 2111 Ejecta, driver gases, and magnetic clouds
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting