Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh42a0779g&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH42A-0779
Other
7519 Flares, 7524 Magnetic Fields
Scientific paper
We use high-resolution, high-cadence images from TRACE together with high quality magnetograms from SOHO/MDI and EUV images from SOHO/EIT to study signatures of magnetic reconnection and attempt to infer associated physical parameters such as the electric field strength in the corona. In this poster we present mainly results from the study of the GOES M1-class flare from NOAA active region 9236 at 2000 Nov 23 23:28 UT, with emphasis on the dynamical development of the flare ribbons in the TRACE images. To estimate the rate of magnetic reconnection, we chose flare ribbons that could easily be separated with binary masks from ejecta and other emission by non-interactive IDL routines. The determined reconnection rate is very noisy, with a correlation time of at most a few seconds. For simple assumptions with standard coronal parameters (B ~ 100 G, np ~ 3 x 109 cm-3 near a strong sunspot), the reconnection appears to be fast, with the inferred inflow velocity a significant fraction of the Alfven velocity. Estimates of the uncertainties of our measurements and analyses are derived from EIT images and simple potential field models. More guidance from coronal imaging of the reconnection regions or Doppler measurements of inflows are needed to sharpen the constraints on the length of the reconnecting current sheets and the coronal electric fields. This work was supported by NASA contracts NAG5-8878, NAG5-10483 (MDI) and NAS5-38099 (TRACE). >http://chippewa.nascom.nasa.gov/gaeng/EOF-Science/
Gaeng T. E.
Saba Julia
Tarbell Theodor
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