Structure and evolution of solar-like oscillaton stars

Thanks to accurate and high-quality observational data of CoRoT (2006) and Kepler (2009), the studies on solar–like oscillating stars have gained now a significant importance in the recent years. With a very large number of the observed oscillation (data) frequencies, we can analyse on the core and close of the core in a star. Furthermore, the fundemantal physical parameters (mass, radius, effective temperature and age) of a star, can be determined by using these sismic constraints and effective temperature coming from the sprectoscopy. These relations are called "scaling relations" in the literature. In this thesis, the solar-like oscillations stars were analysed by using the different stellar interior codes (ANKİ and MESA). First, the frequencies were obtained from the interior model. These model frequencies have been analysed. Consequently, we obtain a decrease in the large separation as a function of frequency. These decreases called as minimum. Therefore, the conventionel scaling relations are have been modified by using these minima. This approach gives very good results for main sequence stars. At the end, we selected fifteen evolved stars the observed parameters are taken from the literature. The models were computed by the MESA evolution code. The new scaling relations are tested on these evolved stars. The age of the system can be obtain with a good accurary (error range is almost 3 Gyr) if the theoretical frequency is correspond well with the observed frequency. Also, the scaling relations with minima are in good agreement with observed values.