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D. Mason (University of Southern California), R. Komm, F. Hill, R. Howe (National Solar Observatory)
We search for a relation between flows below active regions on the Sun and flare events in those active regions. For this purpose, we determine the solar subsurface flows from high-resolution Global Oscillation Network Group (GONG) data using the ring-diagram technique. We then calculate the vorticity of the flows associated with active regions and compare it with the X-ray flare intensity of these regions from the Geostationary Operation Environmental Satellite (GOES). The maximum unsigned vorticity of an active region is correlated with its maximum magnetic flux and the maximum unsigned zonal and meridional vorticity component are also correlated with flare intensity greater than 3.2 \times 10-5~W/m2. Above this threshold, large vorticity values will accompany large magnetic flux for a given flare intensity and larger flare activity will accompany lower magnetic field for a given vorticity value. Active regions with strong flare intensity additionally show a dipolar pattern in the zonal and meridional vorticity component. We define a structure component as a measure of this dipolar pattern and find that it can be represented as a linear function of the logarithm of flare intensity where the slope is linearly dependent on the unsigned flux.
This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. Travel is funded by the University of Southern California.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.