2013/03/26 by Hyeong-Chan Kim · 6 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmological constant #Cosmology #Cosmology and Gravitation Theories #Equation of state #Friedmann–Lemaître–Robertson–Walker metric #Mathematical physics #Physics #Quantum mechanics #Relativity and Gravitational Theory #Scalar field #Theoretical physics #Universe #gr-qc
paper · pdf · doi:10.3938/jkps.63.1675
published in Journal of the Korean Physical Society 63(8), 1675-1680 (Springer Science+Business Media) · 7pages, 1figure
arxiv created 2013/03/26 · openalex publication_date 2013/10/01 · arxiv updated 2013/12/10 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present a new way for describing the solution of the Einstein-scalar field theory with an exponential potential V ∝ e^√ 6 β φ \mathord/ \vphantom √ 6 β φ MPl . \kern-\nulldelimiterspace MPl 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 | L | < 1 \mathord/ \vphantom 1 √ 3 . \kern-\nulldelimiterspace √ 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.