Speaker
Description
The interpretation of solar observations relies critically on our ability to understand how radiation is formed and modified as it propagates through the solar atmosphere. Radiative transfer provides the fundamental framework that connects the physical properties of the plasma such as temperature, velocity, and magnetic field with the observed spectral profiles.
The basic principles of radiative transfer in the solar photosphere and chromosphere are introduced, including the formation of spectral lines under local thermodynamic equilibrium (LTE) and non-LTE conditions. Forward modeling, or spectral synthesis, allows the prediction of observables from atmospheric models, while inversion techniques enable the inference of the underlying physical parameters from spectropolarimetric measurements.
Examples from a variety of solar structures, including the quiet Sun, pores, sunspots, filaments, and arch filament systems, among others, illustrate how radiative transfer techniques are applied in practice. An overview of widely used inversion codes in solar physics is also provided, highlighting their role in the analysis of spectropolarimetric data. This framework provides a coherent view of how radiative transfer techniques are used to extract physical information from the solar atmosphere.
