Scaling solutions from interacting fluids

Nunes, Ana; Mimoso, José P.; Charters, T.

doi:10.1103/physrevd.63.083506

Cited by 32 publications

(30 citation statements)

References 50 publications

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“…On the other hand, the effective energy density (11) associated to the general solution of our interactions has an effective pressure (8) corresponding to a variable modified Chaplygin gas [40][41][42][43][44][45] given by…”

Section: Interacting Modelsmentioning

confidence: 99%

“…[7]; it was mainly motivated to alleviate the coincidence problem in an interacting-quintessence scenario, focusing in an asymptotic attractor behavior for the ratio of the energy densities for the dark components. Since then, many interacting models with numerical and analytical solutions have emerged [8][9][10][11], including interactions with change of sign studied in Refs. [12][13][14].…”

Section: Introductionmentioning

confidence: 99%

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AIC and BIC for cosmological interacting scenarios

2017

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In this work we study linear and nonlinear cosmological interactions, which depend on dark matter and dark energy densities in the framework of general relativity. By using the Akaike information criterion (AIC) and the bayesian information criterion (BIC) with data from SnIa (Union 2.1 and binned JLA), H(z), BAO and CMB we compare the interacting models among themselves and analyze whether more complex interacting models are favored by these criteria. In this context, we find some suitable interactions that alleviate the coincidence problem.

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Section: Interacting Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

AIC and BIC for cosmological interacting scenarios

2017

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“…Thus for W 2 > 9γ/2 (i.e., λ 2 > 3γ), there is a stable fixed point in the interior of the phase space domain. This latter point corresponds to scaling behavior between the matter and scalar field energy-densities [38,40,41,47,48,49]. This attractor solution is characterized by…”

Section: The Dynamics Of Warm Inflationmentioning

confidence: 99%

“…These arise naturally in generalized theories of gravity emerging in the low-energy limits of unification proposals such as super-gravity theories or string theories [36]. On the one hand, after the dimensional reduction to an effective 4-dimensional space-time and the subsequent representation of the theories in the so-called Einstein frame typical polynomial potentials become exponential [37,38]. On the other hand, the theories are then characterised by the existence of a scalar field that couples to all non-radiation fields, with the coupling depending, in general, on the scalar field.…”

Section: Introductionmentioning

confidence: 99%

Asymptotic behavior of the warm inflation scenario with viscous pressure

Mimoso¹,

Nunes²,

Pavón³

2006

Phys. Rev. D

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We analyze the dynamics of models of warm inflation with general dissipative effects. We consider phenomenological terms both for the inflaton decay rate and for viscous effects within matter.We provide a classification of the asymptotic behavior of these models and show that the existence of a late-time scaling regime depends not only on an asymptotic behavior of the scalar field potential, but also on an appropriate asymptotic behavior of the inflaton decay rate. There are scaling solutions whenever the latter evolves to become proportional to the Hubble rate of expansion regardless of the steepness of the scalar field exponential potential. We show from thermodynamic arguments that the scaling regime is associated to a power-law dependence of the matter-radiation temperature on the scale factor, which allows a mild variation of the temperature of the matter/radiation fluid. We also show that the late time contribution of the dissipative terms alleviates the depletion of matter, and increases the duration of inflation. PACS numbers: 98.80.Cq, 47.75+f

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“…The idea of the gradient of the potential generating an interaction between the two perfect fluids, as was mentioned above, is not new and it was analyzed in the literature a long time ago (see e.g. [19] and reference therein). In order to link our formalism of interacting three components with the standard proposal examined within the framework of interacting dark sector we must identify the exchange of energy encoded in Eq.…”

Section: The Modelmentioning

confidence: 99%

Nonbaryonic dark matter and scalar field coupled with a transversal interaction plus decoupled radiation

Chimento

Richarte

2013

Eur. Phys. J. C

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We analyze a universe filled with interacting dark matter, a scalar field accommodated as dark radiation along with dark energy plus a decoupled radiation term within the framework of spatially flat Friedmann-Robertson-Walker (FRW) spacetime. We work in a three-dimensional internal space spanned by the interaction vector and use a transversal interaction Qt for solving the source equation in order to find all the interacting component energy densities. We asymptotically reconstruct the scalar field and potential from an early radiation era to the late dominate dark energy one, passing through an intermediate epoch dominated by dark matter. We apply the χ 2 method to the updated observational Hubble data for constraining the cosmic parameters, contrast with the Union 2 sample of supernovae, and analyze the amount of dark energy in the radiation era. It turns out that our model fulfills the severe bound of Ω φ (z ≃ 1100) < 0.018 at 2σ level, is consistent with the recent analysis that includes cosmic microwave background anisotropy measurements from the Atacama Cosmology Telescope and the South Pole Telescope along with the future constraints achievable by Planck and CMBPol experiments, and satisfies the stringent bound Ω φ (z ≃ 10 10 ) < 0.04 at 2σ level in the big-bang nucleosynthesis epoch.

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Scaling solutions from interacting fluids

Cited by 32 publications

References 50 publications

AIC and BIC for cosmological interacting scenarios

AIC and BIC for cosmological interacting scenarios

Asymptotic behavior of the warm inflation scenario with viscous pressure

Nonbaryonic dark matter and scalar field coupled with a transversal interaction plus decoupled radiation

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