Home > Research > Publications & Outputs > KSVZ axion model with quasidegenerate minima

Associated organisational unit

Electronic data

  • PhysRevD.99.023510

    Final published version, 467 KB, PDF document

    Available under license: CC BY: Creative Commons Attribution 4.0 International License

Links

Text available via DOI:

Keywords

View graph of relations

KSVZ axion model with quasidegenerate minima: A unified model for dark matter and dark energy

Research output: Contribution to journalJournal article

Published
Article number023510
<mark>Journal publication date</mark>15/01/2019
<mark>Journal</mark>Physical Review D
Issue number2
Volume99
Number of pages10
Publication StatusPublished
Early online date4/01/19
<mark>Original language</mark>English

Abstract

We consider the possibility that dark matter and dark energy can be explained by the minimal Kim-Shifman-Vainshtein-Zakharov axion model. This is possible if the lowest energy minimum of the scalar potential has zero energy density, as can occur in theoretical models of vacuum energy cancellation based on spacetime averaging and in models based on energy parity. Dark energy is then understood as being due to the energy density of the metastable electroweak vacuum relative to a second quasidegenerate minimum. The requirement of quasidegenerate minima is a nontrivial condition which completely
determines the form of the potential for a given value of the axion decay constant, fa, and the Pecci-Quinn (PQ) scalar self-coupling, λϕ. The existence of the second quasidegenerate minimum imposes a new
lower bound on the axion decay constant, fa ≥ 2.39 × 10^{10} λ_{\phi}^{−1/4}
GeV. If the PQ symmetry is broken after inflation, then the lower bound on fa implies a lower bound on the amount of axion dark matter,
Ω_{a}/Ω_{dm} ≥ (0.28 − 0.46)λ^{−0.291} , where the range is due to the uncertainty in the amount of axion dark matter produced by vacuum realignment, cosmic strings, and domain walls. Therefore, at least 30% of dark matter
must be due to axions if λ_{\phi} ≲ 1. If axions constitute all of the dark matter then the value of fa, and so the form of the scalar potential, is completely fixed for a given value of λϕ, with only a weak dependence on λ_{\phi}.
This will allow the inflation and postinflation evolution of the model to be quantitatively studied for a given inflation model and dimensionally natural values of λ_{\phi}.