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Inhomogenous Chaotic Inflation

S. Mukherjee·N. K. Dadhich
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Abstract

A chaotic model of the early universe within the framework of the singularity-free solutions of Einstein's equation is suggested. The evolution of our universe at its early stage, starting out as a small domain of the parent universe, is governed by the dynamics of a classical scalar field $ϕ$ . If in any such domain, larger than Planck length,$\dot ϕ$ happens to be very large,$ϕ$ may develop a dominant inhomogeneous mode,leading to an anisotropic inflation of the universe. The particle $ϕ$ is coupled to other particles, which are produced copiously after inflation and these thermalize leading to a rather low temperature universe $(T \geq 10^{4} $ Gev). The electroweak B+L Baryogenesis is assumed to account for the observed baryon asymmetry. The universe now passes through a radiation-dominated phase, leading eventually to a matter-dominated universe, which is isotropic and homogeneous. The model does not depend on the details of Planck scale physics.

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S. Mukherjee, N. K. Dadhich. 1993-10-20. Inhomogenous Chaotic Inflation. https://arxiv.org/abs/gr-qc/9310028

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