Opening a new window for warm dark matter

By T. Asaka, M. Shaposhnikov, A. Kusenko. 2006

182 citations recorded by the source corpus.

We explore the range of parameters for dark-matter sterile neutrinos in an extention of the Minimal Standard Model by three singlet fermions with masses below the electroweak scale (theMSM). This simple model can explain a wide range of phenomena, including neutrino oscillations, baryogenesis, the pulsar velocities, and the early reionization. The presence of two heavier sterile neutrinos and the possibility of entropy production in their decays broadens the allowed range of parameters for the dark-matter sterile neutrinos (or other types of dark matter, for example, the gravitino). In addition, the primordial production of dark matter sterile neutrinos allows to escape most of the constraints.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5a9f24c6944e1662e82468f0a3f7e5647a8148b4

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Citations in the corpus

The Phenomenology of Right Handed Neutrinos (2013, background): “If this production was efficient enough to bring them into thermal equilibrium, their density would be bigger than ΩDM and “overclose” the universe unless they are diluted by entropy production at some later stage [540–542].”
Sterile neutrinos in cosmology (2017, background): “In these decay-production cases, or even the oscillation-production cases, further decays of particles, including related more massive sterile neutrinos, can further “cool” the sterile neutrino dark matter relative to the thermal bath [151, 152, 153, 154].”
Sterile neutrino Dark Matter (2018, background): “5]: N ˘ y 2 S g 0 g (T prod) M Pl m ˚ M keV ’ y S 3:9 g (T prod) M Pl m ˚ M keV ; (57) where g 0 ’3:9 is the late time value of g . The dilution factor Sin Eq. (57) is the same as in50, see e.g. Ref. [471]. If g changes signicantly at the time when the DM production peaks (T˘m ˚=3), a more rened ana”
Warm dark matter in low scale left-right theory (2012, methodology): “• The heavier RH neutrinos N2,3 are the only remaining viable candidates and they play the role of diluters in this scenario [30].”
The Role of Sterile Neutrinos in Cosmology and Astrophysics (2008, background): “ compared to that of active neutrino changes by a factor of S. Therefore, the mixing angle, required to produce the same amount of DM particles today will become S times bigger (for the same DM mass) [38]. Therefore, the computation of sterile neutrino DM production and relation between the mass and”
The Search for Heavy Majorana Neutrinos (2009, methodology): “For example, they can be significantly weakened or evaded if the reheating temperature is low [47, 59], if their density in the Early Universe is diluted by entropy injected at late times [55] or if they have non-standard interactions.”
Dark Matter, Baryogenesis and Neutrino Oscillations from Right Handed Neutrinos (2012, background): “Over the past years, different aspects of the νMSM have been explored using cosmological, astrophysical and experimental constraints [1–3, 6–30].”
Constraints from Ly-α forests on non-thermal dark matter including resonantly-produced sterile neutrinos (2017, background): “Additional production mechanisms exist (see [26]) including production from the decay of a scalar field [27–29] and diluted thermal overproduction [30, 31] to name just a few.”
A White Paper on keV sterile neutrino Dark Matter (2016, background): “WDM also delays the collapse of dwarf-sized haloes and their associated star formation to later epochs.”