Galaxy formation and evolution describe the theoretical processes by which organized stellar systems accrete matter and develop structure over cosmic timescales. Modern cosmological models suggest that galaxies originate from initial density fluctuations in the early universe, collapsing under the influence of gravity. These early stellar clumps grow hierarchically through the continuous accretion of surrounding gas and the merging of smaller satellite galaxies. Within the galaxy's disk, this primordial gas cools and concentrates, forming stars, while the large-scale gravitational potential influences the overall morphology, dictating whether the resulting structure will be a spiral, an elliptical, or an irregular galaxy. Over billions of years, interactions, major mergers, and the subsequent feedback from stellar winds and supernova explosions regulate star formation, dynamically altering the galaxy's gas content, stellar population, and overall structural geometry.