HR: 0800h
AN: SH31A-0222    [Abstracts]
TI: Evidence of Coupled Large-scale Propagating MHD Waves in the EUV Corona
AU: * Wills-Davey, M J
EM: meredith@boulder.swri.edu
AF: Southwest Research Institute, Department of Space Studies 1050 Walnut St., Suite 300, Boulder, CO 80302,
AU: Sechler, M
EM: sechler@boulder.swri.edu
AF: Southwest Research Institute, Department of Space Studies 1050 Walnut St., Suite 300, Boulder, CO 80302,
AU: Sechler, M
EM: sechler@boulder.swri.edu
AF: University of Colorado, Department of Astrophysical and Planetary Sciences Campus Box 391, Boulder, CO 80309,
AU: McIntosh, S W
EM: mcintosh@boulder.swri.edu
AF: Southwest Research Institute, Department of Space Studies 1050 Walnut St., Suite 300, Boulder, CO 80302,
AU: McIntosh, S W
EM: mcintosh@boulder.swri.edu
AF: High Altitude Observatory, National Center for Atmospheric Research 3080 Center Green Dr. CG1, Boulder, CO 80301,
AB: We identify TRACE and SOHO-EIT EUV observations that contain EIT waves or evidence of EIT waves in the form of loop oscillations. In each case, we find instances of a "precursor" to the EIT wave--a much weaker wave pulse that appears instigated by the same source as the EIT wave, and travels in front of the pulse along the same trajectory. In each case, the wave "precursor" leads to some form of coronal dynamics; we observe either loop brightenings or, in one case, the initiation of an EIT wave and a sympathetic coronal mass ejection. These "precursors" are particularly notable in that they travel significantly faster--at least 3 × - 5 × faster--than their corresponding EIT waves, achieving minimum velocities of 1300-1600 km/s. We postulate that these wave "percursors" are, in fact, MHD modes coupled to the EIT waves, and may be a fast- mode-like component correlated with the EIT waves' corresponding slow-mode-like component.
DE: 7509 Corona
DE: 7513 Coronal mass ejections (2101)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting