Cepheid variables are stars that undergo periodic pulsations caused by internal physical processes, producing predictable changes in brightness over time. Astronomers measure these variations using photometric observations; however, continuous data collection is often limited by seasonal visibility, weather, and telescope access. As a result, observational data frequently contain gaps and scatter that obscure underlying patterns. In this project, a physical and computational model simulating Cepheid behavior is developed, and statistical methods are applied to address incomplete and noisy data. These techniques are first tested on model-generated light curves (brightness versus time graphs) and then used to analyze observational data from the American Association of Variable Star Observers (AAVSO) database. From this analysis, key physical properties, including pulsation period and brightness range, are determined.
