The graviscalar quasinormal mode spectrum and late-time power-law tails of a Rastall thick brane are computed numerically, showing that the Rastall parameter λ controls mode lifetimes and tail exponents.
Einstein Static Universe in Rastall Theory of Gravity
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abstract
We investigate stability of the Einstein static solution against homogeneous scalar, vector and tensor perturbations in the context of Rastall theory of gravity. We show that this solution in the presence of perfect fluid and vacuum energy originating from conformally-invariant fields is stable. Using the fix point method and taking linear homogeneous perturbations, we find that the scale factor of Einstein static universe for closed deformed isotropic and homogeneous FLRW universe depends on the coupling parameter $\lambda$ between the energy-momentum tensor and the gradient of Ricci scalar. Thus, in the present model and in presence of vacuum energy, our universe can stay at the Einstein static state past-eternally, which means that the big bang singularity may be resolved successfully in the context of Einstein static universe in Rastall theory.
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Quasinormal modes of scalar perturbations in Rastall thick brane
The graviscalar quasinormal mode spectrum and late-time power-law tails of a Rastall thick brane are computed numerically, showing that the Rastall parameter λ controls mode lifetimes and tail exponents.