Analysis of relativistic compact star models

In this thesis, relativistic modeling of a compact star is examined. For this purpose, a static, spherically symmetric space-time metric was used as the internal geometry while using the Schwarzschild solution as an outer spacetime. Then, a perfect fluid with anisotropic energy momentum tensor, which is observationally more realistic, is considered. The obtained Einstein field equations were solved using the Karmarkar condition. The physical properties of the obtained solutions in both models were examined through observational data of the well-known Cen X-3, LMC X-4, SMC X-4 and Her X-1 neutron stars, which have been studied in the literature. In these studies, some physical quantities, energy conditions, redshift, mass-radius relationship and compactness factor of compact stars were examined. Additionally, the equilibrium and stability states of compact stars were analyzed through the causality condition, Tolman-Oppenheimer-Volkoff equation, Harrisson-Zeldonovich-Novikov condition and relativistic adiabatic index. Both models reveal that stable and balanced compact stars can exist within desired physical limits.