HR: 15:15h
AN: SH33A-06    [Abstracts]
TI: Stereo Observations of Solar Type III Radio Bursts
AU: * Reiner, M J
EM: michael.reiner@gsfc.nasa.gov
AF: Catholic Univ. & NASA/GSCF, Code 674, Greenbelt, MD 20771, United States
AU: Cecconi, B
EM: CECCONI@mesiog.obspm.fr
AF: Observatoire de Paris, LESIA, UMR CNRS 8109 Observatoir de Paris, Meudon, 92195, France
AU: Fainberg, J
EM: joseph.fainberg@nasa.gov
AF: Heliospheric Physics, NASA/GSFC code 673, Greenbelt, MD 20771, United States
AU: Hoang, S
EM: sang.hoang@obspm.fr
AF: Observatoire de Paris, LESIA, UMR CNRS 8109 Observatoir de Paris, Meudon, 92195, France
AU: Kaiser, M L
EM: Michael.Kaiser@nasa.gov
AF: Space Weather Lab., NASA/GSFC code 674, Greenbelt, MD 20771, United States
AU: Makisimovic, M
EM: milan.maksimovic@obspm.fr
AF: Observatoire de Paris, LESIA, UMR CNRS 8109 Observatoir de Paris, Meudon, 92195, France
AU: Goetz, K
EM: Goetz@umn.edu
AF: University of Minnesota, School of Physics and Astronomy University of Minnesota, Minneapolis, MN , United States
AU: Bougeret, J
EM: Jean-Louis.Bougeret@obspm.fr
AF: Observatoire de Paris, LESIA, UMR CNRS 8109 Observatoir de Paris, Meudon, 92195, France
AB: The radio receivers on the STEREO spacecraft provide the first dedicated remote stereoscopic observations of solar and interplanetary radio sources. These observations, from widely separated vantage points, together with simultaneous remote radio observations from Wind/WAVES and Ulysses/URAP, are expected to provide new information and insights about the 3D locations of these radio source regions, as well as their intrinsic radiation characteristics. The STEREO observations allow several ways of doing this, e. g., by using direction-finding techniques to triangulate and directly track the source locations and by using the complementary propagation- time differences. We present here preliminary results from the analysis of timing differences observed for solar type III radio bursts that are simultaneously observed by the two STEREO spacecraft and also by WIND/WAVES and Ulysses/URAP. We will examine how these timing differences vary with observing frequency and with the separation of the various spacecraft, particularly with the separation of the STEREO spacecraft.
DE: 7509 Corona
DE: 7513 Coronal mass ejections (2101)
DE: 7974 Solar effects
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly