Eclipsing binary (EB) is a binary system in which the components are seen eclipsing each other from the Earth. Photometric and spectroscopic observation of EBs show variation on their brightness (light curve) and radial velocity (velocity curve). Light and radial velocity curve analysis provide physical and geometrical parameters of the binary systems and their components, which are very important in stellar evolution studies. These parameters are determined by solving inverse problem, i.e. finding the best-fitting model to the observational curves. Modern EBs modeling programs include detailed physics of stellar atmosphere, geometry, and dynamics of the binary system. One of such models is PHOEBE (PHysics Of Eclipsing BinariEs) 2.3, which offers sophisticated methods to solve the inverse problem. It is solved by computing model curves from initial (estimated) parameters, optimizing them numerically, and sampling the optimized models. We studied CV Boo, a detached EB with a period of 0.847 days, using PHOEBE 2.3. Light curve and radial velocity curves were obtained from the literature. We discuss the steps in finding the solution, present our best solution of the inverse problem, and compare our results with previous studies.