Braneworld models of dark energy

By V. Sahni, Y. Shtanov. 2002

575 citations recorded by the source corpus.

We explore a new class of braneworld models in which the scalar curvature of the (induced) brane metric contributes to the brane action. The scalar curvature term arises generically on account of one-loop effects induced by matter fields residing on the brane. Spatially flat braneworld models can enter into a regime of accelerated expansion at late times. This is true even if the brane tension and the bulk cosmological constant are tuned to satisfy the Randall–Sundrum constraint on the brane. Braneworld models admit a wider range of possibilities for dark energy than standard LCDM. In these models the luminosity distance can be both smaller and larger than the luminosity distance in LCDM. Whereas models with dL ≤ dL(LCDM) imply w = p/ρ ≥ −1 and have frequently been discussed in the literature, models with dL > dL(LCDM) have traditionally been ignored, perhaps because, within the general-relativistic framework, the luminosity distance has this property only if the equation of state of matter is strongly negative (w > t0, where t0 is the present epoch. Such models could help reconcile an accelerating universe with the requirements of string/M-theory.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/733a6b03d312cf40acfccf5627721d5af1028dd5

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Citations in the corpus

Null energy condition and superluminal propagation (2005, background): “A no-go theorem valid in ordinary 4D theories may point towards more exotic scenarii, like for instance the Dvali-Gabadadze-Porrati model [6] where an effective w slightly less than −1 for dark energy can be achieved [7, 8], without manifest pathologies [9].”
Smoothing supernova data to reconstruct the expansion history of the universe (2005, background): “2 As an example, we consider the braneworld dark energy model proposed in Sahni & Shtanov (2003) described by the following set of equations for a flat universe : H2(z) H20 = Ω0m(1+z) 3 + Ωσ + (13) 2Ωl − 2 √ Ωl √ Ω0m(1+z)3 + Ωσ + Ωl + Ωlb Ωσ = 1− Ω0m + 2 √ Ωl(1 + Ωlb) , (14) 2 A very simple model…”
Alternative dark energy models: an overview (2004, methodology): “Although having some unusual properties, this “phantom” behavior is predicted by different approaches as, for example, kinetically driven models [48] and some versions of brane world cosmologies [ 49 ] (see also [50] and references therein).”