Inhomogenous Chaotic Inflation
| dc.creator | Mukherjee, S. | |
| dc.creator | Dadhich, N. K. | |
| dc.date | 1993-10-20 | |
| dc.date.accessioned | 2026-07-07T03:30:10Z | |
| dc.date.available | 2026-07-07T03:30:10Z | |
| dc.description | 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. | |
| dc.description | 12pages, Normal Tex | |
| dc.identifier | https://arxiv.org/abs/gr-qc/9310028 | |
| dc.identifier | http://arxiv.org/abs/gr-qc/9310028 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/35448 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | Inhomogenous Chaotic Inflation | |
| dc.type | text |