Challenges for scaling cosmologies

Abstract

A cosmological model that aims at solving the coincidence problem should show that dark energy and dark matter follow the same scaling solution from some time onward. At the same time, the model should contain a sufficiently long matter-dominated epoch that takes place before acceleration in order to guarantee a decelerated epoch and structure formation. So a successful cosmological model requires the occurrence of a sequence of epochs, namely a radiation era, a matter-dominated era and a final accelerated scaling attractor with ${\Omega }_{\varphi }\simeq 0.7$. In this paper we derive the generic form of a scalar-field Lagrangian that possesses scaling solutions in the case where the coupling $Q$ between dark energy and dark matter is a free function of the field $\varphi$. We then show, rather surprisingly, that the aforementioned sequence of epochs cannot occur for a vast class of generalized coupled scalar field Lagrangians that includes, to our knowledge, all scaling models in the current literature.

14 pages, 3 figures

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• Dark Energy: the equation of state description versus scalar-tensor or modified gravity
• Cosmological Evolution of Interacting Dark Energy Models with Mass Varying Neutrinos
• Cosmological Scaling Solutions and Cross-coupling Exponential Potential

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