The original aim of this work was to study the star spot evolution on contact binaries using the means of numerical modeling. The richnesss of data (Kepler Spacecraft light curves) and practical difficulties (entanglement of the modeled parameters) soon diverted my studies from main topic and forced me to focus on the following questions. My main inquiry was, if the object is truly a binary system. It is possible to answer this question with numerical modeling, i.e. using the Wilson-Devinney code, although several details can influence the best model. One of those, and the subject of my second aim, was to establish which star in the system is the primary (more massive) one. The problem of the primarity of the object can vastly influence the best model. Without spectroscopic data my models were exposed to such possibility. The next issue was the entanglement between the system and the star spot parameters in the Wilson-Devinney code. The size and temperature of star spot do influence the sizes of the binary components, their temperatures and through that, the mass ratio and the fillout factor of the system. Moreover, the latitude of the star spot interacts with the star spot size and its temperature, rendering the search for star spot latitude almost futile. All above problems can be colved completely of partially with the set of methods, the Light Curve Morphology Analysis, which is described in this work.