2016
DOI: 10.1088/1475-7516/2016/04/003
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Dodelson-Widrow production of sterile neutrino Dark Matter with non-trivial initial abundance

Abstract: The simplest way to create sterile neutrinos in the early Universe is by their admixture to active neutrinos. However, this mechanism, connected to the Dark Matter (DM) problem by Dodelson and Widrow (DW), cannot simultaneously meet the relic abundance constraint as well as bounds from structure formation and X-rays. Nonetheless, unless a symmetry forces active-sterile mixing to vanish exactly, the DW mechanism will unavoidably affect the sterile neutrino DM population created by any other production mechanism… Show more

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Cited by 50 publications
(68 citation statements)
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“…We investigate in detail the interplay between the constraints arising from the cosmological and astrophysical observations. Earlier studies on observational properties of frozen-in dark matter in similar models include the case of an ultra-strongly interacting dark matter [16], cosmological, astrophysical and collider constraints on sterile neutrinos [17][18][19][20], and displaced signatures at colliders [21,22]. Frozen-in dark matter has also been used to explain the disagreement between structure formation in cold dark matter simulations and observations [23].…”
Section: Introductionmentioning
confidence: 99%
“…We investigate in detail the interplay between the constraints arising from the cosmological and astrophysical observations. Earlier studies on observational properties of frozen-in dark matter in similar models include the case of an ultra-strongly interacting dark matter [16], cosmological, astrophysical and collider constraints on sterile neutrinos [17][18][19][20], and displaced signatures at colliders [21,22]. Frozen-in dark matter has also been used to explain the disagreement between structure formation in cold dark matter simulations and observations [23].…”
Section: Introductionmentioning
confidence: 99%
“…a vector [732,733] or fermion [679]. In addition, if the sterile-active neutrino mixing is present, then one has to take into account the mechanisms described in section 5.1 as a competing production mode [686].…”
Section: Open Questionsmentioning
confidence: 99%
“…By the orange dashed lines, we indicated bounds based on the Lyman-α constraints based on [538], with primordial distribution functions from scalar decay production, see Sec. 5.3 [663,664,670,686,730,747] and resonant production [314,316,317,691], see Secs. 5.1 and 5.2.…”
Section: What Is the Current Situation?mentioning
confidence: 99%
“…5 assume a DM sector that is predominantly cold with a small fraction of f = 0.2 and 0.1 consisting of a warm species with mTH = 1 keV (where f = ΩWDM/(ΩWDM + ΩCDM) and where mTH is the thermal relic mass of the warm DM component). Such models with subdominant hot or warm DM components can alleviate potential tensions of the velocity function while passing stringent tests from Milky-Way satellite numbers (Schneider 2015;Merle et al 2016) and the Lyman-α forest (Boyarsky et al 2009;Baur et al 2017).…”
Section: Testing the Dark Matter Sectormentioning
confidence: 99%