Supplemental Material
General Relativity and Quantum
Cosmology, abstract
gr-qc/9912036
From: wang mian <mwang@public.xxptt.ha.cn>
Date (v1): Fri, 10 Dec 1999 08:09:30 GMT (11kb)
Date (revised v2): Fri, 3 Mar 2000 14:09:08 GMT (11kb)
The Scalar-Tensor Inflationary Cosmology
Author: Mian Wang
Comments: 17 pages, LaTex, no figure, changed some parameters and
the tables
In this paper the scalar-tensor theory of gravity is assumed to describe the evolution of the universe and the gravitational scalar $\phi$ is ascribed to play the role of inflaton. The theory is characterized by the specified coupling function $\omega(\phi)$ and the cosmological function $\lambda(\phi)$. The function $\lambda(\phi)$ is nearly constant for $0<\phi<0.1$ and $\lambda(1)=0$. The functions $\lambda(\phi)$ and $\omega(\phi)$ provide a double-well potential for the motion of $\phi(t)$. Inflation commences and ends naturally by the dynamics of the scalar field. The energy density of matter increases steadily during inflation. When the constant $\Gamma$ in the action is determined by the present matter density, the temperature at the end of inflation is of the order of $10^{14} GeV$ in no need of reheating. Furthermore, the gravitational scalar is just the cold dark matter that men seek for.
Paper: Source (11kb), PostScript, or Other formats
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Links to: arXiv, gr-qc, /find, /abs (-/+), /9912,
