Skip to main content Accessibility help
  • Print publication year: 2020
  • Online publication date: December 2019

2 - Fundamental Physical Aspects of Radiative Transfer


We consider the fundamental physical processes in stellar atmospheres, together with the basic equations, approximations and techniques used to model them. The coupling of the RT equations with the statistical equilibrium equations is discussed, as well as the role of the atomic properties. The structure equations (equation of state, momentum and energy conservation) that complete the set of equations required to compute a model atmosphere are examined, as well as the broadening mechanisms that change the appearance of the spectral line.