HR: 0800h
AN: SH51C-1223    [Abstracts]
TI: Multi-Spacecraft Modeling of the Topological Evolution of ICMEs
AU: * Liu, Y
EM: liuxying@space.mit.edu
AF: Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, BLDG 37-676A, MIT, Cambridge, MA 02139 United States
AU: Richardson, J D
EM: jdr@space.mit.edu
AF: Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, BLDG 37-676A, MIT, Cambridge, MA 02139 United States
AU: Kasper, J C
EM: jck@space.mit.edu
AF: Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, BLDG 37-676A, MIT, Cambridge, MA 02139 United States
AU: Belcher, J W
EM: jwb@space.mit.edu
AF: Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, BLDG 37-676A, MIT, Cambridge, MA 02139 United States
AU: Hu, Q
EM: qiang.hu@ucr.edu
AF: Institute for Geophysics and Planetary Physics, University of California, 1432 Geology, Riverside, CA 92521 United States
AB: Plasma and magnetic field data from the Helios and Voyager spacecraft are used to investigate the 3D structure of ICMEs. Helios 1 and 2 remained fairly near to each other in the inner heliosphere between 1978 and 1982, while Voyagers 1 and 2 followed each other through the heliosphere out to 10 AU. This period was active in terms of ICME frequency, with about 50 ICMEs observed by the Helios spacecraft and 70 by the Voyagers. If both spacecraft observe the same ICME, we can set lower limits to the longitudinal and azimuthal extents of the event; upper limits can be obtained if an ICME is seen at one spacecraft but missed at the other. The radial variations and sizes of ICMEs can also be obtained as ICMEs pass the spacecraft radially. On a statistical basis, we determine the longitudinal separation and the cross section (radial width plus perpendicular size) of ICMEs. The cross section of the ICMEs deduced above is compared to the numerical solution of the Grad-Shafranov equation fed with 1D observations of the plasma and magnetic field as spatial initial values. The Grad-Shafranov reconstruction of the cross section is tested using multi-spacecraft data since two spacecraft give radial profiles through different parts of an ICME. The association between shock waves and sheath regions of ICMEs will be also investigated.
DE: 2101 Coronal mass ejections (7513)
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2134 Interplanetary magnetic fields
DE: 2139 Interplanetary shocks
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005