The Study of Gravitational Galaxy Clustering in the Expanding Universe Using Thermodynamic Fluctuation Theory

Understanding the formation of the large scale structure is one of the frontiers ofmodern cosmological research. According to the standard scenario, the large scale structure of the universe that we recognize today under the form of galaxies, filaments and sheets is the result of evolution and gravitational growth of small density fluctuations generated at very early times. The study of large scale structure in the expanding universe is currently a challenging problem for cosmologists. As universe expands, galaxies cluster under the influence of motivating gravitational force. Recent observations indicate that while, the large-scale distribution of galaxies appears to be uniform, however, small scale distribution is appreciably influenced by well known tendency towards clustering. Based on a few physically motivated assumptions, Saslaw and Hamilton (1984) arrived at a simple gravitational distribution function, based on the gravitational thermodynamic approximations which we call as gravitational quasi-equilibrium distribution (GQED)