Dissipative quintessence, and its cosmological implications

Abstract

We consider a generalization of the quintessence type scalar field cosmological models, by adding a multiplicative dissipative term in the scalar field Lagrangian, which is represented in an exponential form. The generalized dissipative Klein-Gordon equation is obtained from the variational principle in a covariant form. The energy-momentum tensor of the dissipative scalar field is also obtained from the dissipative Lagrangian. The generalized Friedmann equations in the presence of the dissipative scalar field are obtained for a specific form of dissipation, with the dissipation exponent represented as the time integral of the product of the Hubble function, and of a function describing the dissipative properties of the scalar field. Several cosmological models, corresponding to different choices of the dissipation function, and of the scalar field potential, are considered in detail. The evolutions of the basic cosmological parameters (Hubble function, deceleration parameter etc.) are investigated by using both analytical and numerical techniques. A comparison with the observational data for the Hubble function, and with the predictions of the standard $\Lambda$CDM paradigm is also presented for each dissipative scalar field model. In the large time limit the model describes an accelerating Universe, with the effective negative pressure induced by the dissipative effects associated to the scalar field. Accelerated expansion in the absence of the scalar field potential is also possible, with the kinetic term dominating the expansionary evolution. The dissipative scalar field models describe well the observational data, with the free parameters of the model obtained by a trial and error method. The obtained results show that the dissipative scalar field model offers an effective dynamical possibility for explaining the recent cosmological observational data.

arXiv comment23 pages, 8 figures, accepted for publication in PRD

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