On the spherical collapse model in dark energy cosmologies

By David F. Mota, C. Bruck. 2004

293 citations recorded by the source corpus.

We study the spherical collapse model in dark energy cosmologies, in which dark energy is modelled as a minimally coupled scalar field. We first follow the standard assumption that dark energy does not cluster on the scales of interest. Investigating four different popular potentials in detail, we show that the predictions of the spherical collapse model depend on the potential used. We also investigate the dependence on the initial conditions. Secondly, we investigate in how far perturbations in the quintessence field affect the predictions of the spherical collapse model. In doing so, we assume that the field collapses along with the dark matter. Although the field is still subdominant at the time of virialisation, the predictions are different from the case of a homogeneous dark energy component. This will in particular be true if the field is non-minimally coupled. We conclude that a better understanding of the evolution of dark energy in the highly non-linear regime is needed in order to make predictions using the spherical collapse model in models with dark energy.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a236fa4483c5219118f47fa0c970344f02c74c64

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Citations in the corpus

Spherical collapse in quintessence models with zero speed of sound (2009, background): “give the same description of clustering quintessence as that proposed by [27] and studied, for instance, in [29, 30, 31].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Indeed, in both cases there are no characteristic length scales associated with the quintessence clustering and the spherical collapse remains independent of the size of the object (see [131, 886, 913] for a study of the spherical collapse when cs of quintessence is small but finite).”
Flowing with time: a new approach to non-linear cosmological perturbations (2008, background): “The case of constant equation of state is given by f(τ) = a(τ)−3w, and ΛCDM corresponds to w = −1; 3) Non-vanishing values for bothA 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”