Transition from quintessence to phantom phase in quintom model

Abstract

Assuming the Hubble parameter is a continuous and differentiable function of comoving time, we investigate necessary conditions for quintessence to phantom phase transition in quintom model. For power-law and exponential potential examples, we study the behavior of dynamical dark energy fields and Hubble parameter near the transition time, and show that the phantom-divide-line w=-1 is crossed in these models.

LaTeX, 19 pages, four figures, some minor changes in Introduction, two figures added and the references updated, accepted for publication in Phys. Rev. D

References in corpus (6)

• Cosmological Evolution of a Quintom Model of Dark Energy
• Can dark energy evolve to the Phantom?
• Quintom cosmologies admitting either tracking or phantom attractors
• Avoidance of Big Rip In Phantom Cosmology by Gravitational Back Reaction
• Attractor solutions for general hessence dark energy
• Can universe exit from phantom inflation due to gravitational back reaction?

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