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I am attempting to correlate the surface area (measured number of pixels) covered by plage from K line and H-alpha plage with the variability of the equivalent width in the spectral proxy k2. Correlations between the K line plage and total magnetic flux are also being sought. High resolution k line images are being used to estimate un-measured quiet spicule background. All images are obtained from Big Bear, Kitt Peak and Sacramento Peak Solar Obsevatories via the Internet. Present funding is through Research Corporation. Further funding will be sought through NSF. I am hoping to extend the project at least through Solar Cycle 23.
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