Introduction to MESA stellar evolution code. Description of the possibilities and limitations of
the program. Calibration of numerical parameters in order to obtain results that make
physical sense. Learning how to model different astrophysical objects: molecular clouds
contracting on the main sequence, main sequence stars, red giants, AGB stars, horizontal
branch stars, white dwarfs, black holes. Analysis of physical processes in different phases of
stellar evolution (nuclear reactions, convection, diffusion of chemical elements, energy
transport, mass loss, mixing of matter, angular momentum transport). Modeling the
evolution of binary systems with mass exchange between the components./ Calibration methods for spectroscopic observations of solar flares and prominences obtained
in the optical range. Ultraviolet spectroscopy and photometry of active solar phenomena.
Temporal evolution of stellar and solar flare emissions. Strategies and methods used in the
modelling of solar and stellar flares. One-dimensional models of the active atmosphere of the
Sun and stars. Distributions of non-thermal electrons in the flaring loop (Fokker-Planck).
Diagnostics of star spots based on the photometric modulations. Analysis of solar and stellar
activity cycles. Detection of stellar flares in global surveys of the sky.
