HR: 09:00h
AN: SH11A-05    [Abstracts]
TI: Wind/WAVES and SMEI Observations of ICMEs
AU: * Reiner, M J
EM: reiner@urap.gsfc.nasa.gov
AF: Catholic University - NASA/GSFC, Code 690.2, Greenbelt, MD 20771 United States
AU: Jackson, B V
EM: bvjackson@ucsd.edu
AF: CASS, University of California at San Diego, San Diego, CA 92093 United States
AU: Webb, D F
EM: david.webb@hanscom.af.mil
AF: ISR, Boston College, Hanscom AFB, MA 01731 United States
AU: Kaiser, M L
EM: michael.kaiser@nasa.gov
AF: NASA/GSFC, Code 695, Greenbelt, MD 20771 United States
AU: Cliver, E W
EM: edward.cliver@hanscom.af.mil
AF: Space Vehicles Directorate, Air Force Research Laboratory, Hanscom AFB, MA 01731 United States
AU: Bougeret, J L
EM: jean-louis.bougeret@obspm.fr
AF: LESIA, Paris Observatory, Meudon, 92915 France
AB: The low-frequency (kilometric) radio observations on Wind/WAVES provide important spectral and directional information related to the propagation of ICMEs through interplanetary space. However, up to now there has been no white-light observations with which to compare these low-frequency interplanetary radio observations, beyond the 30 Rs limit of the LASCO field of view. The recently launched Air Force Coriolis spacecraft that includes the Solar Mass Ejection Imager (SMEI), which is the first all-sky camera designed to track ICMEs from the Sun to 1 AU, provides a unique opportunity of simultaneously tracking CMEs, both in white light and in radio, all the way from the corona to 1 AU. 3D reconstruction techniques, utilizing multiple perspective views of the ICME observed by SMEI, represent the propagation and evolution of these density structures through the 3D heliosphere. There are two general ways that the Wind/WAVES radio data can be directly related to the SMEI heliospheric white-light observations. First, since the observed radio frequency depends on the local plasma density in the radio source region and since the interplanetary plasma density falls off with the inverse of the heliocentric distance squared, the observed radio frequency generated by the CME/shock decreases as the type II radio source associated with the CME propagates farther from the Sun. Thus the frequency characteristics of the type II radio emissions provide information on the radial distance of the ICME. Secondly, the low-frequency radio receivers on the Wind spacecraft have the unique capability of providing information on the direction of arrival of the radio emissions and of the size of the radio-emitting region. Both of these results, obtained from analyses of the Wind/WAVES radio observations, will be directly compared with the results from the analyses of the SMEI white-light data for various ICME events.
DE: 7513 Coronal mass ejections
DE: 7534 Radio emissions
DE: 6964 Radio wave propagation
DE: 6969 Remote sensing
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting