Abstract
Within the standard propagation scenario, the flavor ratios of high-energy cosmic neutrinos at neutrino telescopes are expected to be around the democratic benchmark resulting from hadronic sources, $\left( 1 : 1 : 1 \right)_\oplus$. We show how the coupling of neutrinos to an ultralight dark matter complex scalar field would induce an effective neutrino mass that could lead to adiabatic neutrino propagation. This would result in the preservation at the detector of the production flavor composition of neutrinos at sources. This effect could lead to flavor ratios at detectors well outside the range predicted by the standard scenario of averaged oscillations. We also present an electroweak-invariant model that would lead to the required effective interaction between neutrinos and dark matter.
Highlights
We show how the coupling of neutrinos to an ultralight dark matter complex scalar field would induce an effective neutrino mass that could lead to adiabatic neutrino propagation
Cosmological observations have determined the contribution of dark matter (DM) to the energy budget of the Universe with an outstanding precision, the nature of the particles making up this component of the Universe is still unknown
Notice that neutrinos on their path to Earth may pass through voids, but as long as their production site is located within a relatively dense region inside a DM halo and Eq (7) is satisfied at Earth, their initial flavor composition would be preserved at detection
Summary
Cosmological observations have determined the contribution of dark matter (DM) to the energy budget of the Universe with an outstanding precision, the nature of the particles making up this component of the Universe is still unknown. A lower bound on the mass (mDM) comes from the de Broglie wavelength of the DM particle, λdB 1⁄4 2π=ðmDMvÞ, which is required to be smaller than the size of dwarf galaxies. Interesting new effects on the flavor composition could be caused by the coupling of neutrinos to dark matter [27] or to dark energy [28,29,30,31,32,33,34,35] or to the presence of long-range neutrinoelectron interactions [36]. The oscillation pattern of lower energy neutrinos, such as solar, longbaseline, or supernova neutrinos, would not be affected, though For those energies, Δm2=Eν ≫ ΔV, and the standard results are recovered. Note that this energy dependence is a characteristic feature of dimension-three operators
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