The power-law expansion universe and dark energy evolution

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dc.creatorWei, Yi-Huan
dc.date2004-05-19
dc.date2005-02-03
dc.date.accessioned2026-07-07T02:13:14Z
dc.date.available2026-07-07T02:13:14Z
dc.descriptionIn order to depict the transition from deceleration to acceleration expansion of the universe we use a power-law expansion scale factor, $a\sim t^{n_0+bt^m}$, with $n_0$, $b$ and $m$ three parameters determined by $H_0$, $q_0$ 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 $w_X<-1$.
dc.description10 pages, 2 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0405368
dc.identifierhttp://arxiv.org/abs/astro-ph/0405368
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/7746
dc.subjectAstrophysics
dc.titleThe power-law expansion universe and dark energy evolution
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