Interacting Dark Matter and Dark Energy

By G. Farrar, P. Peebles. 2003

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We discuss models for the cosmological dark sector in which the energy density of a scalar field approximates Einstein's cosmological constant and the scalar field value determines the dark matter particle mass by a Yukawa coupling. A model with one dark matter family can be adjusted so the observational constraints on the cosmological parameters are close to but different from what is predicted by the ΛCDM model. This may be a useful aid to judging how tightly the cosmological parameters are constrained by the new generation of cosmological tests that depend on the theory of structure formation. In a model with two families of dark matter particles the scalar field may be locked to near zero mass for one family. This can suppress the long-range scalar force in the dark sector and eliminate evolution of the effective cosmological constant and the mass of the nonrelativistic dark matter particles, making the model close to ΛCDM, until the particle number density becomes low enough to allow the scalar field to evolve. This is a useful example of the possibility for complexity in the dark sector.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f869a3658aa785f36e6508cfc2512e92faad1193

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Citations in the corpus

Observational constraints on an interacting dark energy model (2009, background): “Various forms for Qc have been put forward (see, e.g. Wetterich (1995); Amendola (1999); Billyard & Coley (2000); Zimdahl & Pavon (2001); Farrar & Peebles (2004); Chimento et al. (2003); Olivares et al. (2005); Koivisto (2005); Sadjadi & Alimohammadi (2006); Guo et al. (2007); Boehmer et al.…”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “A Yukawa-like interaction was investigated (Farrar and Peebles 2004; Das et al. 2006), pointing out that coupled dark energy behaves as a fluid with an effective equation of state w −1, though staying well defined and without the presence of ghosts (Das et al.”
Interacting dark energy in the early 2020s: A promising solution to the H0 and cosmic shear tensions (2019, background): “[130–239], for a recent comprehensive review see [200]).”
Cluster number counts dependence on dark energy inhomogeneities and coupling to dark matter (2005, background): “A non-minimal coupling of the quintessence field to dark matter is therefore worth investigating (Amendola 2000; Mainini & Bonometo 2004; Amendola & Tocchini-Valentini 2002a; Farrar & Peebles 2004; Amendola & Tocchini-Valentini 2002b; Wetterich 1995; Tocchini-Valentini & Amendola 2002).”
The speed of the ‘bullet’ in the merging galaxy cluster 1E0657−56 (2007, background): “…model of particle physics not only predict dark matter candidates in the form of new elementary particles, but also additional (long-range) fields which may couple differently to the dark matter particles and ordinary baryons (e.g. Damour et al. 1990; Farrar & Peebles 2004; Gubser & Peebles 2004).”
Dark energy from mass varying neutrinos (2003, background): “nishes, and subsequent evolution would be like normal pressureless matter. Also interesting to consider is the case of a steeper than quadratic potential, leading to positive pressure. One might hope [38,41,42,52] that obtaining dark matter and dark energy from the same source would help address the”
Equivalence Principle Implications of Modified Gravity Models (2009, background): “elementary baryons and dark matter particles are coupled to the scalar with different strengths [39, 40, 41, 42, 43, 44].”