HR: 1330h
AN: SH43A-09    [Abstracts]
TI: Orientation and Configuration of Magnetic Flux Ropes: From Sun to 1 AU
AU: * Hu, Q
EM: qiang.hu@ucr.edu
AF: University of California, Riverside, 1432 Geology, Riverside, CA 92521 United States
AU: Dasgupta, B
EM: Brahmananda.Dasgupta@ucr.edu
AF: University of California, Riverside, 1432 Geology, Riverside, CA 92521 United States
AB: The Corona Mass Ejections (CMEs) are commonly modeled as magnetic flux ropes. We examine a simple and intuitive means of inferring orientation of flux rope axis from coronagraph images of halo CMEs, based on the hypothesis of flux rope configuration. Preliminary results in connection with Dst index will be presented. The interplanetary counterparts of CMEs, the ICMEs, detected in-situ by spacecraft ACE and Wind, etc, have been examined in much more details. In particular, we present the Grad-Shafranov (GS) reconstruction technique, which represents an objective means of obtaining the axis orientation of a flux rope. In addition, it is capable of deriving 2 1/2 dimensional cross-section of a cylindrical flux rope from single-spacecraft measurements. We will compare the axis orientation of flux-rope CMEs and their corresponding ICMEs. We attempt to establish the relationship between the CMEs and the Interplanetary Magnetic Field (IMF) conditions upon their arrival at 1 AU, thus to assess their geoeffectiveness. We propose to seek connections among observables of CMEs at sun, the corresponding ICMEs, and the geomagnetic storms. Theoretical work on three-dimensional generalized GS type equation will be discussed.
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2134 Interplanetary magnetic fields
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7894 Instruments and techniques
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly