AAS 200th meeting, Albuquerque, NM, June 2002
Session 65. The Magnetic Structure of CMEs
SPD Topical Session Oral, Wednesday, June 5, 2002, 2:30-4:00pm, 4:15-6:00pm, Ruidoso/Pecos

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[65.06] Using Potential Field Models to Learn About CME Coronal Context and Consequences

J.G. Luhmann, Y. Li (Space Sciences Lab, U. of California Berkeley), C.N. Arge (CIRES, U of Colorado and NOAA-SEC), X-P. Zhao, Y. Liu (Stanford University), O.C. St. Cyr (NASA GSFC and Catholic University ), N. Rich (NRL and Interferometrics Inc.)

To date, searches for photospheric field signatures of CMEs have produced evidence of involvement of active regions exhibiting nonpotential character. Evidence of the role of larger-scale photospheric fields has been elusive, though state-of-the-art models of CMEs generally require what should be observable changes. Motivated by the apparent interaction of fields on active region and helmet streamer scales in many coronagraph images, we modify this search to instead consider the inferred relationships between active regions and the larger scale fields of helmet streamers derived from potential field source surface models. These comparisons suggest CMEs occur in conjunction with certain helmet streamer configurations where the streamer is sensitive to the involved active region. Thus the key for observers and modelers may lie not in large scale photospheric field changes, but in combinations of active region and large scale fields that are sensitive to reconfiguration by eruption.

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.