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Published online by Cambridge University Press: 24 December 2019
This chapter considers a selection of numerical methods developed since 1960s for solving radiative transfer (RT) problems in stellar atmospheres and in all other diluted media where non-LTE effects are important. Special emphasis is put on the solution of the radiative transfer equation (RTE) when the source function is given, because its so-called formal solution constitutes a necessary step in any iterative procedure for the solution of more general RT problems. The application of different methods to the spectral line formation the line(s) radiation field and thestatistical equilibrium (SE) equation(s) for the atomic-level populations involved is discussed for both linear and nonlinear problems.
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