The Sterile-Active Neutrino Flavor Model: the Imprint of Dark Matter on the Electron Neutrino Spectra. (arXiv:1812.07182v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lopes_I/0/1/0/all/0/1">Ilídio Lopes</a>
Contact interactions between sterile neutrinos and dark matter particles in a
hidden sector have been suggested as a good solution to simultaneously resolve
the dark matter problem and anomalies in neutrino experiments. In this
non-standard particle physics model, sterile and active neutrinos change their
through vacuum oscillations and matter (or Mikheyev–Smirnov–Wolfenstein)
oscillations, in which the latter mechanism of flavor oscillation depends
strongly on the concentration of dark matter in the Sun’s core. We found that a
large concentration of dark matter in the Sun’s interior changes substantially
the shape of ${rm ^8B}$ and $rm hep$ electron neutrino spectra, but has an
insignificant impact on the other neutrino spectra (i.e., $rm pp$, $rm pep$,
$rm ^7Be$ and $rm ^{15}O$, $rm ^{13}N$ and $rm ^{17}F$). The strength of
the interaction of the dark matter particles with neutrinos depends on an
effective coupling constant, $G_chi$, which is an analog of the Fermi constant
for the hidden sector. By using the latest $rm ^8B$ solar neutrino flux, we
found that $G_chi$ must be smaller than $rm 0.5times 10^9$ $G_{rm F}$ for
this particle physics model to be in agreement with the data.
Contact interactions between sterile neutrinos and dark matter particles in a
hidden sector have been suggested as a good solution to simultaneously resolve
the dark matter problem and anomalies in neutrino experiments. In this
non-standard particle physics model, sterile and active neutrinos change their
through vacuum oscillations and matter (or Mikheyev–Smirnov–Wolfenstein)
oscillations, in which the latter mechanism of flavor oscillation depends
strongly on the concentration of dark matter in the Sun’s core. We found that a
large concentration of dark matter in the Sun’s interior changes substantially
the shape of ${rm ^8B}$ and $rm hep$ electron neutrino spectra, but has an
insignificant impact on the other neutrino spectra (i.e., $rm pp$, $rm pep$,
$rm ^7Be$ and $rm ^{15}O$, $rm ^{13}N$ and $rm ^{17}F$). The strength of
the interaction of the dark matter particles with neutrinos depends on an
effective coupling constant, $G_chi$, which is an analog of the Fermi constant
for the hidden sector. By using the latest $rm ^8B$ solar neutrino flux, we
found that $G_chi$ must be smaller than $rm 0.5times 10^9$ $G_{rm F}$ for
this particle physics model to be in agreement with the data.
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