Second Model

Today I finished the second model that I mentioned in the last post. After doing some tests on a couple of stars, it looks like this one is much better than the last one(and required much less math,time,graphs,pretty much everything). The approach we took to this one was to take the aforementioned B and V band magnitudes. We then took the difference in these(called the color index) and used this number to calculate the temperature of the star. We then used just the V magnitude, the distance of the star, and whats called a bolometric correction constant(pretty much just a constant to convert from the visual range to the whole range) to calculate the luminosity of the star. We then used an equation published in a paper that uses the temperature and luminosity that we just calculated to find the inner and outer edges of the habitable zone. The reason I think that this model was much better than the last is mostly because of the fact that the equation from the paper takes into account the greenhouse effect which has a large effect on the boundaries. Also because this model only uses the B and V magnitudes, it will be much easier to use than the model that requires the data set to be complete. I will update in a few days once we run all of the stars through the model and get to see how well it works on the whole set of them.


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