The power-law expansion universe and dark energy evolution

2004/05/19 by Yi-Huan Wei, Wei, Yi-Huan
Computer Science · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #Computational Physics and Python Applications #Cosmology and Gravitation Theories #FOS: Physical sciences #astro-ph

paper · pdf · doi:10.48550/arxiv.astro-ph/0405368

10 pages, 2 figures

openalex publication_date 2004/05/19 · arxiv created 2005/02/03 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

In order to depict the transition from deceleration to acceleration expansion of the universe we use a power-law expansion scale factor, a∼ t^n₀+btm, with n₀, b and m three parameters determined by H₀, q₀ and z_T. For the spatially flat, isotropic and homogeneous universe, such a scale factor leads to the results that the dark energy density is slowly changing currently, and predicts the equation of state w_X changes from w_X>-1 to w_X

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