Can dark energy evolve to the Phantom

By A. Vikman. 2004

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Dark energy with the equation of state $w(z)$ rapidly evolving from the dustlike ($w\ensuremath{\simeq}0$ at $z\ensuremath{\sim}1$) to the phantomlike ($\ensuremath{-}1.2\ensuremath{\lesssim}w\ensuremath{\lesssim}\ensuremath{-}1$ at $z\ensuremath{\simeq}0$) has been recently proposed as the best fit for the supernovae Ia data. Assuming that a dark energy component with an arbitrary scalar-field Lagrangian $p(\ensuremath{\varphi},{\ensuremath{\nabla}}_{\ensuremath{\mu}}\ensuremath{\varphi})$ dominates in the flat Friedmann universe, we analyze the possibility of a dynamical transition from the states $(\ensuremath{\varphi},\stackrel{\ifmmode \dot{}\else \textperiodcentered \fi{}}{\ensuremath{\varphi}})$ with $w\ensuremath{\ge}\ensuremath{-}1$ to those with $wl\ensuremath{-}1$ or vice versa. We have found that generally such transitions are physically implausible because they are either realized by a discrete set of trajectories in the phase space or are unstable with respect to the cosmological perturbations. This conclusion is confirmed by a comparison of the analytic results with numerical solutions obtained for simple models. Without the assumption of the dark energy domination, this result still holds for a certain class of dark energy Lagrangians, in particular, for Lagrangians quadratic in ${\ensuremath{\nabla}}_{\ensuremath{\mu}}\ensuremath{\varphi}$. The result is insensitive to topology of the Friedmann universe as well.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f62d7473a9e1ae05719fc772676cf5e9b20a0c4c

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In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

The clustering of galaxies in the SDSS‐III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large‐scale two‐point correlation function (2012, background): “In the framework of gen- eral relativity, a single fluid, or a single scalar field without higher derivatives, cannot cross this threshold since it would become gravitationally unstable (Feng et al. 2005; Vikman 2005; Hu 2005; Xia et al 2008), requiring at least one extra degree of freedom.”