Cosmological evolution of a quintom model of dark energy

By Zongkuan Guo, Yun-Song Piao, Xinmin Zhang, Yuan-zhong Zhang. 2004

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We investigate in this Letter the cosmological evolution of a dark energy model with two scalar fields where one of the scalar has canonical kinetic energy and another scalar has negative kinetic energy term. For such a system with exponential potentials we find that during the evolution of the universe the equation of state w changes from w greater than or equal to -1 to w < -1, which is consistent with the recent observations. A phase-plane analysis shows that the "phantom"-dominated scaling solution is the stable late-time attractor of this type of models. (C) 2005 Elsevier B.V. All rights reserved.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2255adaf4baf62d6b5f26f64e3d42a1c770e890a

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Citations in the corpus

Phantom energy traversable wormholes (2005, background): “The evolving dark energy with an equation of state ω crossing −1 during its evolution was dubbed “Quintom” [35, 37, 38], as it is different from the quintessence or phantom fields in the determination of the evolution and fate of the universe.”
Observational constraints on teleparallel dark energy (2011, background): “The first is to modify the content of the universe by introducing the dark energy sector, which can be based on a canonical scalar field (quintessence) [6–22], a phantom field [23–28], or on the combination of both these fields in a unified scenario called quintom [29–35] (see [36] for a review).”
Hořava–Lifshitz dark energy (2009, background): “However, one still cannot distinguish between this model and alternative models that allow for the realization of wDE < −1 phase, such are modified gravity [40, 41] or models with phantom [34, 42, 43] or quintom fields [44, 45, 46, 47].”