Coupled three-form dark energy

Abstract

Cosmology with a three-form field interacting with cold dark matter is considered. In particular, the mass of the dark matter particles is assumed to depend upon the amplitude of the three-form field invariant. In comparison to coupled scalar field quintessence, the new features include an effective pressure contribution to the field equations that manifests both in the background and perturbation level. The dynamics of the background is analyzed, and new scaling solutions are found. A simple example model leading to a de Sitter expansion without a potential is studied. The Newtonian limit of cosmological perturbations is derived, and it is deduced that the coupling can be very tightly constrained by the large-scale structure data. This is demonstrated with numerical solutions for a model with nontrivial coupling and a quadratic potential.Comment: 13 pages, 6 figure

Cosmological evolution with interaction between dark energy and dark matter

“…It can be shown [32], that for α, β, γ 1 , γ 2 ≥ 0 and γ 1 = γ 2 this inequality is always satisfied. For A 2 > 8B we find the solution…”

The anisotropy of a three- and a one-form

“…Three-fields are among the competitors for "the" model of inflation [3,4]; they support a perfectly isotropic background [5,6]; they inflate easily and exhibit some very peculiar dynamics [7]; they can drive a late-time "dark energy" era with peculiar matter interactions [8,9]; and, last but not least, they support couplings with a variety of other forms, including the obvious one-form case.…”

Non-Gaussianity in multiple three-form field inflation

“…[17][18][19].) Despite the success of inflation driven by scalar fields, three-forms provide a viable alternative (and a viable model of dark energy) [20][21][22][23][24][25][26][27]. Inflation considering multiple three-form fields has been investigated in the past as these models are important due to their connection to string theory scenarios [28].…”