Reconstruction of f(T) gravity from the Holographic dark energy

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Abstract

Among different candidates to play the role of Dark Energy (DE), modified gravity has emerged as offering a possible unification of Dark Matter (DM) and DE. The purpose of this work is to develop a reconstruction scheme for the modified gravity with \(f(T)\) action using holographic energy density. In the framework of the said modified gravity we have considered the equation of state of the Holographic DE (HDE) density. Subsequently we have developed a reconstruction scheme for modified gravity with \(f(T)\) action. Finally we have obtained a modified gravity action consistent with the HDE scenario.

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A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state

(2010)

It is extraordinary that a number of observations indicate that we live in a spatially flat, low matter density Universe, which is currently undergoing a period of accelerating expansion. The effort to explain this current state has focused attention on cosmological models in which the dominant component of the cosmic energy density has negative pressure, with an equation of state \(w \ge -1\). Remarking that most observations are consistent with models right up to the \(w=-1\) or cosmological constant (\(\Lambda\)) limit, it is natural to ask what lies on the other side, at \(w<-1\). In this regard, we construct a toy model of a ``phantom'' energy component which possesses an equation of state \(w<-1\). Such a component is found to be compatible with most classical tests of cosmology based on current data, including the recent type 1a SNe data as well as the cosmic microwave background anisotropy and mass power spectrum. If the future observations continue to allow \(w<-1\), then barring unanticipated systematic effects, the dominant component of the cosmic energy density may be stranger than anything expected.

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Essentials of k-essence

Paul J. Steinhardt, C. Armendáriz-Picón, V. Mukhanov (2000)

We recently introduced the concept of "k-essence" as a dynamical solution for explaining naturally why the universe has entered an epoch of accelerated expansion at a late stage of its evolution. The solution avoids fine-tuning of parameters and anthropic arguments. Instead, k-essence is based on the idea of a dynamical attractor solution which causes it to act as a cosmological constant only at the onset of matter-domination. Consequently, k-essence overtakes the matter density and induces cosmic acceleration at about the present epoch. In this paper, we present the basic theory of k-essence and dynamical attractors based on evolving scalar fields with non-linear kinetic energy terms in the action. We present guidelines for constructing concrete examples and show that there are two classes of solutions, one in which cosmic acceleration continues forever and one in which the acceleration has finite duration.

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Kinetically Driven Quintessence

Takahiro Okabe, Takeshi Chiba, Masahide Yamaguchi (1999)

Recently, a novel class of models for inflation has been found in which the inflationary dynamics is driven solely by (non-canonical) kinetic terms rather than by potential terms. As an obvious extension, we show that a scalar field with non-canonical kinetic terms alone behaves like an energy component which is time-varying and has negative pressure presently, i.e. quintessence. We present a model which has a constant equation of state, that is, a ``kinetic'' counterpart of the Ratra-Peebles model of a quintessence field with a potential term. We make clear the structure of the phase plane and show that the quintessential solution is a late-time attractor. We also give a model for the ``phantom'' component which has an equation of state with \(w=p/\rho <-1\).