Computer Science
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........29h&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF COLORADO AT BOULDER, 1995.Source: Dissertation Abstracts International, Volume: 57-04, Section: B,
Computer Science
Alpha Flux
Scientific paper
The purpose of this thesis was to model the Lyman alpha variability observed from the Sun based on the evolution of magnetic active regions. The approach I have used was to convolve the time evolution of the magnetic flux of active regions with an appropriate response function to mimic the observed variability of the observed Lyman alpha. This convolution with a response function acts to spread the effect of the magnetic flux from active regions through time to represent the effect of the decay and diffusion of magnetic plages with an active network. A single response function for all active regions was empirically derived to fit observations when only a few active regions were present on the solar disk. This response function has an e-folding growth time of 17.24 days, and an e-folding decay time of 100.0 days. This e-folding time is comparable to a simple seven-rotation smoothing used in Lean and Skumanich (1983). This response function was convolved with magnetic data for 112 active regions spanning approximately two and a half years. The resulting model for the Lyman alpha flux has a reduced chi-squared of 0.983, which is indicative of a good fit between the model results and the SME-observed Lyman alpha. This supports the hypothesis that an active network made up of decayed remnants of previous active regions has a significant effect on the Lyman alpha emission. The model results were only weakly sensitive to the assumed rise and decay rate of the response function. The amplitude of the response function, however, is an important parameter, and a single value does not work well for all active regions. The amplitude is assumed to vary as a decreasing function of the total magnetic active region flux.
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