GAMMA DOR BİLEŞENLİ ÇİFT SİSTEMLER
Proje no. 630 · Durum: Kapanmış · 2017
Özet
<p>In recent years, theoretical and observational researches on the possible relationships between the dominant pulsational periods and the absolute parameters and the orbital periods of the binary have been</p><p>an important field of study. Mass, Radius, and effective temperatures, plus local gravity, density, and deformation on their surface structures due to tidal forces, of the eclipsing binary components can be</p><p>obtained by photometric and spectroscopic observations. We determine the astrophysical parameters of the eclipsing binary components with an accuracy of 1-5%. The continuous and accurate photometric</p><p>observation was obtained by the space missions Kepler. The relationship between the pulsational properties and binarity effects was not established for the γ Dor and δ Scuti stars in the eclipsing</p><p>binaries, located on the main-sequence. New studies have shown that the pulsational period increases as the orbital period longer for the γ Dor and δ Scuti stars. Due to the limited data, the effects of the</p><p>binarity on the pulsation, as well as the relation between the pulsation and astrophysical parameters could not be established yet. The relationship between the pulsational and orbital periods has been</p><p>confirmed by the space missions observations. Although the relationship between the pulsational periods and the orbital periods for the δ Scuti stars have been investigated both theoretically and observationally, we have a little amount of information on the distances between the components, their masses, and radii, surface potentials, surface gravities, etc. In order to answer those and such questions, it is necessary to carry out precise photometric and spectroscopic observations of binary systems containing pulsating variables. In the framework of this project, it is very much important to carry out the photometry and the spectroscopy of the binary systems with pulsating components in order to determine their absolute parameters and, in doing so, to find solutions to this important astrophysical problem.</p>