Finishing up the first model

So today we finished the first model. What we ended up doing to fix the problem from the last post was to use Stefan-Boltzmann law to relate temperature and flux. What we assumed was that the inner boundary was when the temperature was at 373 K (boiling point of water) and that the outer edge was at 273 K (freezing point of water). What we also did was assume that a planet would be similar to Earth and would reflect 30% of the flux that it receives(the planet’s albedo). Using this reflection, the temperature assumptions, and the Stefan-Boltzmann law we were then able to define the boundaries of the habitable zone. After doing that, we could use the calculations we were doing from before, and this time we got very good results for the inner boundary and alright results for the outer boundary(compared to other predictions of the zone). The reason I think the outer boundary results were somewhat poor was because our model is pretty simplistic and only takes into account the solar flux, but in reality an entire planet would do a better job at conserving heat, and thus could still have liquid water farther out than our model predicts. We are going to make another model soon that we will compare to this one, but hopefully the new model will be just as accurate if not more, but require less data, because currently, not all of the stars have the required data for the first model.


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