SH43B-4202:
What Do EUV Dimmings Tell Us About CME Topology?
Thursday, 18 December 2014
Barbara J Thompson, NASA Goddard Space Flight Center, Greenbelt, MD, United States, Marc L DeRosa, Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA, United States, Richard R Fisher, Goddard Spaceflight Center, Code670, Greenbelt,MD, MD, United States, Larisza D Krista, NOAA/SWPC, Boulder, CO, United States, Ryun Young Kwon, George Mason University Fairfax, School of Physics, astronomy and Computational Sciences, Fairfax, VA, United States, James P Mason, University of Colorado at Boulder, Boulder, CO, United States, M. Leila Mays, NASA/GSFC, Greenbelt, MD, United States, Nariaki Nitta, Lockheed Martin Adv Tech, Lockheed Martin STAR Labs, Palo Alto, CA, United States, Neel Savani, George Mason University Fairfax, Fairfax, VA, United States and Matthew John West, Royal Observatory of Belgium, Brussels, Belgium
Abstract:
Large-scale coronal EUV dimmings, developing on timescales of minutes to hours in association with a flare or filament eruption, are known to exhibit a high correlation with coronal mass ejections. However, it is not clear why some CMEs have dimmings and some do not, nor is it clear how these dimmings relate to CME topology. The inner coronal coverage of SDO AIA and STEREO EUVI, combined with the extended field of view of PROBA2's SWAP imager, allow us the opportunity to map the topology of a dimming region in three dimensions into an erupting CME. Although the location and extent of a dimming region appears to be the best indicator of the inner "footprint" of a CME, the correlation is far from perfect. However, dimmings can provide vital clues about the development and 3D kinematics of a CME. This is particularly important as we are entering an extended period of time where STEREO coronagraph images will not always be available, and therefore the 3D properties of a CME will be difficult to deduce. Therefore, understanding the inner coronal manifestations of a CME can provide clues to its structure and dynamics, even without multi-viewpoint coronagraph observations. We present the results of this combined analysis effort, along with a discussion of how dimmings can be used in forecasting CME directions.
