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The main mode of energy transport through the photosphere is via radiation, i.e., photons.We consider how these photons are created and destroyed and how the energy flows outward.We build on the material from the previous two chapters and formulate the mathematical integral needed to calculate the spectrum of a star.Convection is considered briefly, mainly because it introduces velocity fields into the photosphere.
Fourier transforms and convolutions occur in dealing with spectrographs, stellar spectra, and many of the physical processes found in stellar photospheres.This chapter puts in place the Fourier tools we need.
On our way to calculating model stellar photospheres (next chapter), we need to study the continuous absorption.The main contributors are neutral hydrogen for hotter stars and the negative hydrogen ion for cooler, solar-type, stars.The physics and equations are developed for calculating the continuous absorption coefficient as it is needed in the solution of the transfer equation.