Stellar physics

The central task of our study of the active close binary stars (CBS) is to improve the existing computer programs for modeling and interpretation of photometric and spectroscopic observations of CBS, brown dwarves and exoplanets, by incorporating more physical details into the models. We expect to make improvements to the treatment of the reflection effect, gravitational and limb darkening, as well as in the modeling of circumstellar structures – the accretion disk, gas stream, jets and active regions with spots; the effects of the rotational distortion and asynchronous rotation of the stars and of the accretion disk on the radial velocity curves, and the effects of radial and non-radial oscillations of components on the light curves of CBS. The modeling of interacting CBS allows us to determine the physical characteristics of the circumstellar gas, contributing to our understanding of mass transfer, accretion processes, formation of active regions and instabilities inside the accretion disk. We will explore the dynamical evolution of contact CBS of W UMa type and the conditions of their stability. The development of new methods will allow us to analyze quasi-periodic signals that cannot be adequately studied using Fourier analysis. We plan to study the observed properties of small-scale phenomena in the Solar photosphere and to obtain an improved abundance of manganese, as well as to study the telluric lines in the Solar spectrum.