HR: 09:00h
AN: SH51B-04    [Abstracts]
TI: In-situ and Numerical Modeling Prospects for Multipoint ICME Observations Featuring the 22 May 2007 STEREO Event
AU: * Lynch, B J
EM: blynch@ssl.berkeley.edu
AF: Space Sciences Laboratory, Univ. of California, Berkeley 7 Gauss Way, Berkeley, CA 94270, United States
AU: Li, Y
EM: yanli@ssl.berkeley.edu
AF: Space Sciences Laboratory, Univ. of California, Berkeley 7 Gauss Way, Berkeley, CA 94270, United States
AU: Huttunen, K E
EM: huttunen@ssl.berkeley.edu
AF: Space Sciences Laboratory, Univ. of California, Berkeley 7 Gauss Way, Berkeley, CA 94270, United States
AU: Antiochos, S K
EM: antiochos@nrl.navy.mil
AF: E. O. Hulburt Center for Space Research, Naval Research Laboratory 4555 Overlook Ave. SW, Washington, DC 20375, United States
AU: DeVore, C R
EM: devore@lcp.nrl.navy.mil
AF: Laboratory for Computational Physics and Fluid Dynamics, Naval Research Laboratory 4555 Overlook Ave. SW, Washington, DC 20375, United States
AU: Luhmann, J G
EM: jgluhman@ssl.berkeley.edu
AF: Space Sciences Laboratory, Univ. of California, Berkeley 7 Gauss Way, Berkeley, CA 94270, United States
AB: We will present recent 3D MHD simulation results of eruptive flux-rope formation via the magnetic breakout mechanism to provide a theoretical/modeling context for multipoint in-situ observations. Many generic observational CME properties are reproduced by this idealized eruption as it propagates through the low corona (~10 R_\odot). Recently, STEREO observed a "classic" flux-rope ICME on 22 May 2007 with different in- situ field and plasma signatures seen at each spacecraft. The same event was also seen by WIND and ACE, arriving at L1 arriving a few hours before either STEREO A or B. We will describe a preliminary analysis of the large-scale heliospheric structure of the ICME flux-rope utilizing the linear, force-free cylinder model fits to the in- situ magnetic field rotations in order to determine the ICME's relative simplicity and/or consistency with the standard Magnetic Cloud cartoon picture. A comparison between the data, the derived in-situ cylinder orientations at three spacecraft, and the CME large-scale magnetic structure inferred from the MHD simulation results in the low corona show a reasonable qualitative agreement. BJL would like to acknowledge support from NSF ATM-0621725 as a SHINE Postdoc, and thank the STEREO, WIND and ACE teams for making their data readily available.
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2134 Interplanetary magnetic fields
DE: 7513 Coronal mass ejections (2101)
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting