Abstract
Using extreme ultraviolet (EUV) images of the solar corona, we have carried out a region-by-region study of the association of coronal emission of Fe IX-Fe XVI with Ca II K plage areas and intensities reported in Solar-Geophysical Data. We find that emission is dependent on the area and brightness of the plage, with specific correlations varying with the temperature of formation of the emitting coronal ion. If confirmed and extended, this approach may provide a means of estimating coronal EUV levels associated with solar activity and ultimately a proxy method that is more accurate than the sole use of the centimetric radio flux for estimating the coronal component of solar EUV emission.
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