Initial conditions for the scalaron dark matter

Abstract

The scalaron of the metric $f(R)$ gravity can constitute dark matter if its mass is in the range $4\text{meV}\lesssim m\lesssim 1\text{MeV}$. We give an overview of such $f(R)$ gravity theory minimally coupled to the Standard Model. Similarly to other dark-matter models based on scalar fields, this model has the issue of initial conditions. Firstly, the initial conditions for the scalaron are to be tuned in order to produce the observed amount of dark matter. Secondly, the primordial spatial inhomogeneities in the field are to be sufficiently small because they generate entropy (or isocurvature) perturbations, which are constrained by observations. We consider these issues in the present paper. The initial conditions for the scalaron presumably emerge at the inflationary stage. We point out that the homogeneous part of the scalaron initial value is largely unpredictable because of quantum diffusion during inflation. Thus, to account for the observed amount of dark matter, one has to resort to anthropic considerations. Observational constraints on the primordial spatial inhomogeneity of the scalaron are translated into upper bounds on the energy scale of inflation, which happen to be low but not too restrictive.

19 pages, 1 figure, errors and typos corrected, matches the published version

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• Interactions of the scalaron dark matter in $f(R)$ gravity
• Is it possible to separate baryonic from dark matter within the $\Lambda$-CDM formalism?
• Generalized black-bounces solutions in f(R) gravity and their field sources
• Effective scalaron--photon interaction in $f(R)$ gravity
• Universality in static spherically symmetric solutions of f(R) gravity
• Theoretical and observational constraints on early dark energy in $F(R)$ gravity