calculations, we input the distribution of temperature, density and composition and predict the spectrum that we will see, including emission and absorption lines. We vary the input parameters until we find models that produce predictions that agree with the observations. The results of these calculations are not unique, but they do give us a feel for what processes are important in stellar atmospheres. The more observational data we can predict with the models, the more confident we can be that the temperatures, densities and compositions we derive are close to the actual ones.

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