HR: 14:00h
AN: SH33A-01    [Abstracts]
TI: The SECCHI Experiment on the STEREO Mission
AU: * Howard, R A
EM: russell.howard@nrl.navy.mil
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Moses, J D
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Vourlidas, A
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Newmark, J S
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Socker, D G
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Wang, D
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Plunkett, S P
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Baugh, R
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: McMullin, D R
EM:
AF: Naval Research Lab, E.O. Hulburt Center for Space Research, Washington, DC 20375, United States
AU: Davila, J M
EM:
AF: NASA/GSFC, Code 682, Greenbelt, ME 20771, United States
AU: Thompson, W T
EM:
AF: NASA/GSFC, Code 682, Greenbelt, ME 20771, United States
AU: Lemen, J R
EM:
AF: Lockheed Martin Solar & Astrophysics Lab, 3251 Hanover Street, Palo Alto, CA 94304, United States
AU: Wuelser, J
EM:
AF: Lockheed Martin Solar & Astrophysics Lab, 3251 Hanover Street, Palo Alto, CA 94304, United States
AU: Harrison, R A
EM:
AF: CCLRC, Rutherford Appleton Laboratory, Chilton Didcot, OX11 OQX, United Kingdom
AU: Waltham, N R
EM:
AF: CCLRC, Rutherford Appleton Laboratory, Chilton Didcot, OX11 OQX, United Kingdom
AU: Davis, C J
EM:
AF: CCLRC, Rutherford Appleton Laboratory, Chilton Didcot, OX11 OQX, United Kingdom
AU: Eyles, C J
EM:
AF: CCLRC, Rutherford Appleton Laboratory, Chilton Didcot, OX11 OQX, United Kingdom
AU: Eyles, C J
EM:
AF: University of Birmingham, School of Physics and Astronomy Edgbaston, Birmingham, B15 2TT, United Kingdom
AU: Defise, J
EM:
AF: Centre Spaatiale de Liege, Avenue du Pre Aily, Angleur, B-4031, Belgium
AU: Halain, J
EM:
AF: Centre Spaatiale de Liege, Avenue du Pre Aily, Angleur, B-4031, Belgium
AU: Bothmer, V
EM:
AF: Institut fur Astrophysik, Friedrich-Hund-Platz Universitat Gottingen, Gottingen, 37077, Germany
AU: Delaboudiniere, J
EM:
AF: Institute dâ€ââ€& #382;¢Astrophysique Spatiale, Université Paris â€ââ‚&# 172;Å“ Sud / CNRS, Orsay, F-91405, France
AU: Auchere, F
EM:
AF: Institute dâ€ââ€& #382;¢Astrophysique Spatiale, Université Paris â€ââ‚&# 172;Å“ Sud / CNRS, Orsay, F-91405, France
AU: Mercier, R
EM:
AF: Institute dâ€ââ€& #382;¢Optique, Laboratoire Charles Fabry, Orsay, F-91403, France
AU: Ravet, M F
EM:
AF: Institute dâ€ââ€& #382;¢Optique, Laboratoire Charles Fabry, Orsay, F-91403, France
AB: The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO) mission is a suite of remote sensing instruments consisting of an extreme ultraviolet (EUV) imager, two white light coronagraphs, and two telescopes that comprise the heliospheric imager. SECCHI will observe coronal mass ejections (CMEs) from their birth at the sun, through the corona and into the heliosphere. A complete instrument suite is being carried on each of the two STEREO spacecraft, which will provide the first sampling of a CME from two vantage points. The spacecraft, launched 25 October 2006, are orbiting the Sun, one Ahead of the Earth and the other Behind, each separating from Earth at about 22 degrees per year. The varying separation means that we will have different observational capabilities as the spacecraft separate and therefore differing science goals. The primary science objectives all are focused on understanding the physics of the CME process their initiation, 3D morphology, propagation, interaction with the interplanetary medium and space weather effects. By observing the CME from multiple viewpoints with UV and coronagraphic telescopes and by combining these observations with radio and in-situ observations from the other instruments on STEREO as well as from other satellites and ground based observatories operating at the same time, answers to some of the outstanding questions will be obtained. We will show some of the initial results.
DE: 2101 Coronal mass ejections (7513)
DE: 2102 Corotating streams
DE: 2129 Interplanetary dust
DE: 2164 Solar wind plasma
DE: 2169 Solar wind sources
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly