HR: 1340h
AN: SH43A-1145    [Abstracts]
TI: Global 3-D Solar Wind Analysis of Halo CMEs Using Interplanetary Scintillation (IPS) Remote Sensing and its Comparison at Mars
AU: * Boyer, J A
EM: jaboyer@ucsd.edu
AF: Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093 United States
AU: Jackson, B V
EM: bvjackson@ucsd.edu
AF: Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093 United States
AU: Buffington, A
EM: abuffington@ucsd.edu
AF: Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093 United States
AU: Hick, P P
EM: pphick@ucsd.edu
AF: Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093 United States
AU: Yu, Y
EM: yyu@cs.ucsd.edu
AF: Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093 United States
AU: Crider, D H
EM: crider@cua.edu
AF: Catholic University of America, 106 Driftwood Dr., Gibsonville, NC 27249 United States
AB: The Interplanetary Scintillation (IPS) process allows observation of the inner heliospheric response to CMEs in scintillation level and velocity. With the help of our colleagues in STELab, Japan, we have developed near real time access of these data for use in space weather forecasting. We use a 3D reconstruction technique that obtains perspective views from outward-flowing solar wind as observed from Earth by iteratively fitting a kinematic solar wind model using the IPS observations. This 3D modeling technique permits us to reconstruct the density and velocity structure of CMEs, and other interplanetary transient structure at low resolution (with a one day cadence, and at a 20 deg. latitudinal and longitudinal heliographic resolution). Here we explore the use of this technique to reproduce the solar wind pressure observed at Mars following the aftermath of halo (Earth-directed) CMEs. These CMEs include one that erupted from the Sun on May 27, 2003 and another on October 28, 2003 both of which produced a large response at Mars. In addition we explore the response at Mars and our reconstruction of "backside" (as seen from Earth) halo CMEs.
UR: http://cass185.ucsd.edu/forecast/index_v_n.html
DE: 2101 Coronal mass ejections (7513)
DE: 2102 Corotating streams
DE: 2780 Solar wind interactions with unmagnetized bodies
DE: 5421 Interactions with particles and fields
DE: 6929 Ionospheric physics (1240, 2400)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005