Abstract
We argue that an interacting scalar-fermion distribution can be used to demonstrate the cosmic acceleration in General Relativity. The interaction is of Yukawa nature and it drives the fermion density to decay with cosmic time. The consistency of the model is established through, (a) a generalization of the O m ( z ) parameter, the present matter density contrast of the universe and (b) a comparison of theoretical results with observational data, using a Markov Chain Monte Carlo code. A simple toy model of unified cosmic expansion history is also discussed, where the universe goes through transitions between subsequent epochs with different patterns of cosmic expansion. These patterns impose some constraints on the scalar-fermion interaction profile and on the overall cosmological dynamics.
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