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Initial conditions for the scalaron dark matter
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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.
Forward citations
Cited by 4 Pith papers
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Effective scalaron--photon interaction in $f(R)$ gravity
In the Jordan-frame treatment of f(R) gravity the scalaron-photon effective coupling vanishes for m much less than loop-particle masses because the classical-trace diagrams cancel the Fujikawa anomaly term.
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Scalaron dark matter dynamics: effects of Higgs non-minimal coupling to gravity
Adding Higgs non-minimal coupling ξ modifies the scalaron-Higgs trilinear term, yielding scalaron dark matter masses in 2.7 meV–0.7 MeV (misalignment case) or 3.6 meV–770 meV (interaction-dominated cases) plus an LHC-...
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Interactions of the scalaron dark matter in $f (R)$ gravity
For scalaron dark matter in f(R) gravity, the two-photon decay rate is confirmed at one loop, the resulting extragalactic background spectrum is derived, and the thermal scalaron abundance is shown to be negligible.
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Universality in static spherically symmetric solutions of f(R) gravity
Static spherically symmetric vacuum solutions of three f(R) models have universal rescaled scalaron and metric-alpha profiles for large Mµ, with common near-center asymptotics ζ=1.
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