Year: 2013
Type: article
Abstract: We present a new way for describing the solution of the Einstein-scalar field theory with an exponential potential $$V \propto e^{{{\sqrt 6 \beta \varphi } \mathord{\left/ {\vphantom {{\sqrt 6 \beta \varphi } {M_{Pl} }}} \right. \kern-\nulldelimiterspace} {M_{Pl} }}}$$ in a spatially-flat Friedmann-Robertson-Walker space-time, where β is a constant characterizing the interactions and M Pl is the Planck mass. We introduce a new time variable, L, which may vary in (−1, 1). The new time clearly represents the state of the universe because the equation of state at a given time takes the simple form w = −1 + 2L 2. The universe will inflate when $$\left| L \right| < {1 \mathord{\left/ {\vphantom {1 {\sqrt 3 }}} \right. \kern-\nulldelimiterspace} {\sqrt 3 }}$$ . For β ≥ 1, the universe ends with its evolution at L = β. This implies that the equation of state at the end of the universe is nothing but w = −1 + 2β 2. For β ≥ 1, the universe ends at L = 1, where the equation of state of the universe is one. On the other hand, the universe always begins with w = 1 at L = ±1.
DOI: 10.3938/jkps.63.1675
Author: Hyeong-Chan Kim
Institution: Korea National University of Transportation
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: green
OpenAlex ID: W1980822902