In this model, we do not assume that the sun is a perfect blackbody, but rather that the temperature is a function of the wavelength. Using a previous paper, I used two linear functions to model this. This model requires 3 parameters from published data in the program that generates the spectrum: the slope of the two lines, and the point at which they intersect (wavelength with the lowest effective temperature). For this first graph, I used slopes of -1 and 2.1, with the minimum occurring at 1625Å. The emission with a minimum temperature of 4350K can then be calculated:
Using programs similar to the previous ones, I was able to construct a histrogram for the two wavelengths 1515Å and 1569Å to compare to previously published data. The graphs on the left were calculated with 1600Å band data, on the right with 1700Å data. The upper line is the quiet sun, the lower is active regions. Minimum at 1600Å
Minimum at 1650Å
Compare this to previously published data (Brekke):
Also, I can calculate the temperature of each pixel using this new model:
Min at 1600Å above, 1650Å below.
Here's the data represented in a histogram for the quiet sun and active regions
Median temperatures for each pixel, with error bars of 1 standard deviation. Min=1600 on left, 1650 on right Quiet Regions:
Active Regions: