The rôle of the interaction in crossing the phantom divide line in the Chaplygin gas model is discussed. We obtain some general properties of the interactions that allow the model to arrive at phantom divide line. We show that these properties put some conditions on the ratio of dark matter to dark energy density. PACS: 98.80.-k, 98.80.Jk

It is explored that if dominant component of content of the future universe behaves as Chaplygin gas, voilation of other energy conditions (null energy condition, weak energy condition and dominant energy condition) can be avoided if " strong energy condition " is obeyed. In the investigations, here, two cases arise. In one case, universe expands with acceleration leading to finite energy densi...

Remark that real flows should be non-isentropic. The constancy of the entropy is not compatible once shock waves develop. It is only expected that the amplitude of oscillations for the entropy are of cubic order with respect to those of the flow. There is one notable exception, that of a Chaplygin gas, whose pressure has the form p(ρ, s) = g(s)− f(s)/ρ ; then the entropy remains constant even b...

In this letter, I have proposed a model of variable modified Chaplygin gas and shown its role in accelerating phase of the universe. I have shown that the equation of state of this model is valid from the radiation era to quiessence model. The graphical representations of statefinder parameters characterize different phase of evolution of the universe. All results presented in the letter concer...

The Generalized Chaplygin Gas (GCG) with the equation of state p = − A ρ was recently proposed as a candidate for dark energy in the Universe. In this paper we confront the GCG with SNIa data using avaliable samples. Specifically we have tested the GCG cosmology in three different classes of models with (1) Ωm = 0.3, ΩCh = 0.7; (2) Ωm = 0.05, ΩCh = 0.95 and (3) Ωm = 0, ΩCh = 1, as well as a mod...

Anisotropic cosmological models with a generalized Chaplygin gas in a Finsler space-time geometry are considered and a class of exact solutions as well as cosmological parameters behaviors are studied. Moreover, the viability and stability criteria for a general solution are also discussed.