Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2917w&link_type=abstract
American Astronomical Society Meeting 210, #29.17; Bulletin of the American Astronomical Society, Vol. 39, p.140
Other
Scientific paper
Two kinds of large energetic phenomena occurring in the solar atmosphere referred as eruptive event (X-class flares with associated CMEs) and confined event (X-class flares without associated CMEs) are comparatively studied by investigating 4 X-class events in each of the two types. Both sets of events are selected to have very similar intensity (X1.0 to X3.6) and duration (rise time less than 13 minutes and decaying time less than 9 minutes) in soft X-ray observations. We find no difference in the total magnetic flux of the photospheric source regions for the two sets of events. However, we find that the occurrence of eruption (or confinement) is sensitive to the displacement of the location of the energy release, which is defined as the distance between the flare site and the flux-weighted magnetic center of the source active region. The displacement is 6 to 17 Mm for confined events, but is as large as 22 to 37 Mm for eruptive events. In other words, confined events occur closer to the magnetic center while the eruptive events tend to occur closer to the edge of active regions. Further, we have used potential-field source-surface model (PFSS) to infer the 3-D coronal magnetic field above source active regions. For each event, we calculate the coronal flux ratio of low corona (< 1.1 R&sun;) to high corona (>= 1.1 R&sun;). We find that the confined events have a lower coronal flux ratio (< 5.7), while the eruptive events have a higher flux ratio(> 7.1). These results imply that a stronger overlying arcade field may prevent energy release in the low corona from being eruptive, resulting in flares without CMEs. A CME is more likely to occur if the overlying arcade field is weaker.
Wang Yuming
Zhang James J.
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