Inhomogenous Chaotic Inflation

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 $\varphi$ . If in any such domain, larger than Planck length,$\dot{\varphi }$ happens to be very large,$\varphi$ may develop a dominant inhomogeneous mode,leading to an anisotropic inflation of the universe. The particle $\varphi$ is coupled to other particles, which are produced copiously after inflation and these thermalize leading to a rather low temperature universe $(T\ge {10}^4$ 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.