Holographic Dark Energy in Brans-Dicke Theory

Abstract

In this paper, the holographic dark energy model is considered in Brans-Dicke theory where the holographic dark energy density ${\rho }_{\Lambda }=3c^2{M}_{pl}^2{L}^{-2}$ is replaced with ${\rho }_h=3c^2\Phi (t)L^{-2}$. Here $\Phi (t)=\frac{1}{8\pi G}$ is a time variable Newton constant. With this replacement, it is found that no accelerated expansion universe will be achieved when the Hubble horizon is taken as the role of IR cut-off. When the event horizon is adopted as the IR cut-off, an accelerated expansion universe is obtained. In this case, the equation of state of holographic dark energy $w_h$ takes a modified form $w_h=-1/3(1+\alpha +\frac{2}{c}\sqrt{{\Omega }_h})$. In the limit $\alpha \to 0$, the 'standard' holographic dark energy is recovered. In the holographic dark energy dominated epoch, power-law and de Sitter time-space solutions are obtained.

7 pages, 1 figure, match the published version

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• Dynamics of dark energy
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• Holographic dark energy in Brans-Dicke theory
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