HR: 1340h
AN: SH13A-0300    [Abstracts]
TI: Magnetic Structure of Halo CMEs and Corresponding ICMEs
AU: * Krall, J
EM: jonathan.krall@nrl.navy.mil
AF: Plasma Physics Division, Naval Research Laboratory, Code 6790, Washington, DC 20375-5346 United States
AU: Yurchyshyn, V B
EM: vayur@bbso.njit.edu
AF: Big Bear Solar Observatory, New Jersey Institute of Technology, Big Bear City, CA 92314 United States
AU: Chen, J
EM: james.chen@nrl.navy.mil
AF: Plasma Physics Division, Naval Research Laboratory, Code 6790, Washington, DC 20375-5346 United States
AB: The detailed connection between a halo coronal mass ejection (CME) and its corresponding ``interplanetary CME'' (ICME) is an area of active study. Using the erupting flux rope model [1-2], we present model/data comparisons for multiple CME/ICME events near the sun (using coronagraph image data) and in the heliosphere (using in situ measurements). We find that the near-Sun magnetic configuration, as obtained from a match of the model to the observed halo-CME morphology, is closely related to the ICME magnetic configuration, as determined by matching the model ICME to the in situ magnetic field and plasma measurements. The differences between the near-Sun flux-rope orientation parameters and the near-Earth orientation parameters are noted in each case. These indicate that, typically, the apex of the flux rope is deflected by 5-10 degrees as the flux rope expands outwards to 1 AU. [1] Chen, J. 1996, JGR, 101, 27499 [2] Krall, J. et al., 2000, ApJ, 539, 964
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 7513 Coronal mass ejections (2101)
DE: 7959 Models
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005