Abstract
A pedagogical treatment to the effect of cosmological constant in the big-bang model is presented. It is argued that quantum fluctuations of the vacuum contributes to the cosmological constant and, essentially, leads to the cosmological constant problem. The equation of state corresponding to the cosmological constant is derived using the conservation of energy-momentum tensor in the Friedman models. The epoch after which the cosmological constant starts dominating over the non-relativistic matter is calculated. The evolution of the expansion factor as a function of cosmic time is discussed for the flat model case when A is positive. The ensuing age of the universe since the birth of high redshift QSOs is compared with the ages of the globular clusters. Collapse of a spherical dust ball and its virialization is considered. The flatness problem in the presence of a non-zero cosmological constant is discussed.
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