Linear and nonlinear perturbations in dark energy models

By Luca Amendola. 2003

170 citations recorded by the source corpus.

I review the linear and second-order perturbation theory in dark energy models with explicit interaction to matter in view of applications to N-body simulations and non-linear phenomena. Several new or generalized results are obtained: the general equations for the linear perturbation growth; an analytical expression for the bias induced by a species-dependent interaction; the Yukawa correction to the gravitational potential due to dark energy interaction; the second-order perturbation equations in coupled dark energy and their Newtonian limit. I also show that a density-dependent effective dark energy mass arises if the dark energy coupling is varying.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/35b6355acd6d316053216b11b6e1cdfa11b467bb

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In Astronomy and Astrophysics

In Statistical and Nonlinear Physics

Citations in the corpus

Flowing with time: a new approach to non-linear cosmological perturbations (2008, background): “ and ΛCDM corresponds to w = −1; 3) Non-vanishing values forboth A and B occur when particles’ geodesics are modiﬁed, as it happens for instance when the DM particles couple to some light scalar ﬁeld [36, 37, 38] or in Scalar-Tensor theories of gravity [39, 40]. In the latter case, if α(ϕ) represent”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “06 (at 95% CL for a constant coupling and an exponential potential) [152, 62, 47, 59], or possibly more [720, 711] if neutrinos are taken into account or for more realistic timedependent choices of the coupling.”
Hydrodynamical N-body simulations of coupled dark energy cosmologies (2008, methodology): “…investigated, for β(φ) given by a constant, both in its background and linear perturbation features (Wetterich 1995; Amendola 2000) as well as with regard to the effects on structure formation (Amendola 2004; Pettorino & Baccigalupi 2008) , and via a first N-body simulation (Macciò et al. 2004).”
Structure formation in inhomogeneous dark energy models (2004, background): “3 C O U P L E D QU I N T E S S E N C E Let us now look at the case when the scalar field has a coupling with all or part of the dark matter (see for e.g. Amendola 2004; Tocchini-Valentini & Amendola 2002; Amendola & Tocchini-Valentini 2002).”