Transition from quintessence to the phantom phase in the 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 powerlaw 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 ω = −1 is crossed in these models.

On the resolution of cosmic coincidence problem and phantom crossing with triple interacting fluids

“…This approximation can be saturated to equality by inserting a dimensionless parameter (say λ i ). Thus we can write [20] (see [21] for more exotic expressions for Q i )…”

Quintom Potential from Quantum Anisotropic Cosmological Models

“…Writing (6) in canonical form, L canonical = Π qq − NH and substituting the energy density for the barotropic fluid, we can find the Hamiltonian density H in the usual way…”

“…There are many works in the literature that deals with this type of problems, but in a general way, and not with a particular ansatz, one that considers dynamical systems [12,13,20]. One special class of potentials used to study this behaviour corresponds to the case of the exponential potentials [4,6,9,26,28] for each field, where the corresponding energy density of a scalar field has the range of scaling behaviors [29,30], i.e, it scales exactly as a power of the scale factor like, ρ φ ∝ a −m , when the dominant component has an energy density which scales in a similar way. There are other works where other type of potentials are analyzed [1,9,15,19,20,23,24,31].…”

Thermodynamics in Closed Universe With Entropy Corrections

“…where Υ i indicate the interacting parameters which may be taken in terms of Hubble parameter or energy density of DM or DE or in terms of both 44,45) .…”