Massive sterile neutrinos as warm dark matter

By A. Dolgov, S. Hansen. 2000

321 citations recorded by the source corpus.

Abstract We show that massive sterile neutrinos mixed with the ordinary ones may be produced in the early universe in the right amount to be natural warm dark matter particles. Their mass should be below 40 keV and the corresponding mixing angles sin22θ>10−11 for mixing with νμ or ντ, while mixing with νe is slightly stronger bounded with mass less than 30 keV.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/503fb824aa828318ce856e1b847585873708d32d

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In Nuclear and High Energy Physics

Citations in the corpus

Constraints on sterile neutrinos as dark matter candidates from the diffuse X-ray background (2005, methodology): “4 of Dolgov & Hansen (2002).”
Sterile neutrino Dark Matter (2018, background): “few keV, they are a viable DM candidate [31{38]. Sterile neutrino DM interacts much weaker than ordinary neutrinos. These particles can leave imprints in X-ray spectra of galaxies and galaxy clusters [33,34,39{41]. Moreover, they decay [42] and X-ray observations provide 5 bounds on their parameters”
Gravitational probes of dark matter physics (2017, background): “Though the connection between astrophysical measurements and particle physics models of dark matter is recognized for particular models (notably, sterile neutrinos [31, 32, 33, 34, 35]), the full potential is perhaps not appreciated in the broader context.”
A facility to search for hidden particles at the CERN SPS: the SHiP physics case (2015, background): “and the energy of the emitted photon is fixed to be Eγ = 1 2MN which means that one expects a monochromatic line in the spectra of dark matter-dominated objects (galaxies and galaxy clusters) [726, 733, 734].”
Lyman-alpha constraints on warm and on warm-plus-cold dark matter models (2008, methodology): “In this case the distribution can be roughly approximated by the renormalized Fermi-Dirac distribution of Eq.”
Flavor structures of charged fermions and massive neutrinos (2019, background): “Given the fact that such sterile particles are unable to thermalize in an easy way, the simplest mechanism for their production is either via non-resonant active-sterile neutrino oscillations [104, 603] or through resonant active-sterile neutrino oscillations in the presence of a non-negligible lept”
The Phenomenology of Right Handed Neutrinos (2013, background): “With few exceptions [312], these simulations assume that the DM distribution is proportional to a Fermi-Dirac distribution [494].”
The Role of Sterile Neutrinos in Cosmology and Astrophysics (2008, background): “of sterile neutrino ∼ 1 eV [27] will not be discussed here. Sterileneutrinosincosmologyandastrophysics 7 bigger. This radiative decay would produce a narrow line e.g. in the diﬀuse X/γ-ray background [30, 32]. This gives a restriction on the mixing angle θ2 1 .1.8×10−5 keV M 1 5 , (12) meaning tha”
A White Paper on keV sterile neutrino Dark Matter (2016, background): “If the sterile neutrino is a main ingredient of the DM, it is potentially detectable in various X-ray observations [324, 566, 567].”
Dark Matter, Baryogenesis and Neutrino Oscillations from Right Handed Neutrinos (2012, background): “The shadowed (blue) region is excluded by the non-observation of an X-ray line from N1 decay in DM dense regions [7, 13, 90, 91, 106–113].”
Sterile neutrinos in cosmology (2017, background): “[27] also discussed diffuse X-ray constraints on nonresonantly produced sterile neutrino dark matter.”