We study FRW homogeneous cosmological solutions in the bigravity extension of the recently found ghost-free massive gravity. When the additional extra metric, needed to generate the mass term, is taken as nondynamical and flat, no homogeneous flat FRW cosmology exists. We show that, when the additional metric is a dynamical field a perfectly accetable FRW solution exists. Solutions fall in two branches. In the first branch the massive deformation is equivalent to an effective cosmological constant determined by the graviton mass. The second branch is quite rich: we have FRW cosmology in the presence of a gravitational'' fluid. The control parameter $\xi$ is the ratio of the two conformal factors. When $\xi$ is small, the evolution is similar to GR and interestingly the universe flows at late time towards an attractor represented by a dS phase.

### FRW Cosmology in Ghost Free Massive Gravity from Bigravity

#### Abstract

We study FRW homogeneous cosmological solutions in the bigravity extension of the recently found ghost-free massive gravity. When the additional extra metric, needed to generate the mass term, is taken as nondynamical and flat, no homogeneous flat FRW cosmology exists. We show that, when the additional metric is a dynamical field a perfectly accetable FRW solution exists. Solutions fall in two branches. In the first branch the massive deformation is equivalent to an effective cosmological constant determined by the graviton mass. The second branch is quite rich: we have FRW cosmology in the presence of a gravitational'' fluid. The control parameter $\xi$ is the ratio of the two conformal factors. When $\xi$ is small, the evolution is similar to GR and interestingly the universe flows at late time towards an attractor represented by a dS phase.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11697/6425
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