HR: 1330h
AN: SP23A-09    [Abstracts]
TI: CME Population Distributions: Science Facilitated by the VSO
AU: * Davey, A
EM: ard@boulder.swri.edu
AF: Southwest Research Institute, Dept of Space Science 1050 Walnut St. Suite 400, Boulder, CO 80302 United States
AU: Wills-Davey, M
EM: meredith@boulder.swri.edu
AF: Southwest Research Institute, Dept of Space Science 1050 Walnut St. Suite 400, Boulder, CO 80302 United States
AU: Gurman, J
EM: gurman@gsfc.nasa.gov
AF: NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics Code 682.3, Greenbelt, MD 20771 United States
AU: Bogart, R
EM: rick@rick.stanford.edu
AF: Stanford University, Dept of Physics, Stanford, CA 94305 United States
AU: Dimitoglou, G
EM: george@esa.nascom.nasa.gov
AF: NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics Code 682.3, Greenbelt, MD 20771 United States
AU: Hill, F
EM: hill@noao.edu
AF: National Solar Observatory, 920 N. Cherry Ave, Tucson, AZ 85726 United States
AU: Hourcle, J
EM: oneiros@grace.nascom.nasa.gov
AF: NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics Code 682.3, Greenbelt, MD 20771 United States
AU: Martens, P
EM: martens@solar.physics.montana.edu
AF: Montana State University, Dept of Physics, Bozeman, MT 59717 United States
AU: Suarez Sola, I
EM: igor@noao.edu
AF: National Solar Observatory, 920 N. Cherry Ave, Tucson, AZ 85726 United States
AU: Tian, K
EM: ktian@stanford.edu
AF: Stanford University, Dept of Physics, Stanford, CA 94305 United States
AU: Wampler, S
EM: swampler@noao.edu
AF: National Solar Observatory, 920 N. Cherry Ave, Tucson, AZ 85726 United States
AU: Yoshimura, K
EM: yosimura@solar.physics.montana.edu
AF: Montana State University, Dept of Physics, Bozeman, MT 59717 United States
AB: The Virtual Solar Observatory (VSO) exists to simplify and unify access to Solar Physics data. It provides a single interface to a broad spectrum of data types and sources which previously would have required considerable effort to collect. Using this ability to combine data sources, we access the entire SOHO/LASCO CME catalog and compare it with GOES observations of X-ray flares. Because we consider these data in their entirety, we find several instances where the results of less extensive studies may show unintentional selection effects. As a subpopulation, we specifically consider LASCO-observed halo CMEs. In agreement with previous studies, we find halo CMEs are the bulk of the fastest events. This selection effect is consistent with randomly-distributed CMEs extending over wide angles (>120 degrees). We also examine the lack of slower halo CMEs; otherwise randomly-distributed events are rarely Earth-directed. While geometric and Thomson scattering issues make less-energetic halo CMEs hard to detect, this dearth of slow observations may represent an additional seeing threshold. The lack of low-energy detections may account for the disparity in LASCO.s prediction of Kp ≥ 6 vs. Kp ≥ 5 geomagnetic storms.
DE: 7513 Coronal mass ejections
DE: 7594 Instruments and techniques
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly