General characteristics of γ dor stars

From the 1960s onwards, subclasses of pulsating stars began to emerge in detail. However, almost all the stars on the HR diagram are composed of pulsating variables. The most active region known as the Cepheid instability strip where in the main sequence and the vicinity δ Scuti and γ Dor pulsating stars is located. These stars have been the source of many studies in recent years. Both stars are mixed together. However, we know from the studies that the two stars group pulsating reasons are different from each other. In this thesis, the physical properties of γ Dor stars were examined in detail and the literature data of the stars in this scope were collected and a small γ Dor catalog was tried to be created. In this study particular emphasis is on γ Dor stars, which are binary star components. Besides, the relation between pulsating periods and absolute parameters of single stars and binary star members was investigated. The effect of binarity on the pulsating was investigated. In this context, a threshold value of about 12 days was found in the orbit period. In addition, the gravitational effect of the companion star was also examined. As a result, the characteristics of γ Dor stars are studied and the mystery of the stars are tried to be removed.