Magnetic activity and the enhanced 5303 A emission in solar active regions

Analysis of the intensity maps of Fe XIV emission at lambda = 5303 Angstrom obtained from the observations of ground-based coronagraphs during the sun spot minimum period 1985 and 1986 shows the persistent presence of localize d strong emissions. Typical emission intensities associated with the active regions were found to be about 5 to 20 times stronger than the unperturbed corona. Using Stanford magnetograms rye identified strong magnetic held gr adients in those active regions. with a minimum threshold gradient of 3 x 1 0(-5) G km(-1), associated with such strong emissions. From our sample we i nfer that the flux emergence within or in the vicinity of 3 persistent acti ve region seems to play an important role in the activity associated with t he enhancement in 5303 Angstrom emission.