Neutrinos and dark matter

Ibarra, Alejandro

doi:10.1063/1.4915588

Cited by 5 publications

(10 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Specifically, we explore the possibility of directly detecting DM in existing large neutrino detectors at energies much higher than presently considered. After further motivating this idea, we explore 1 For recent reviews, see [1,2].…”

Section: Introductionmentioning

confidence: 99%

“…Recent experiments have, however, significantly constrained this space for such particles (also called WIMPS). 1 When combined with results from indirect DM searches and colliders, it is fair to say that credible reasons for seriously considering "non-WIMP" and possibly non-thermal candidates for DM exist (for a review, see [3]). In addition, we note that Big Bang Nucleosynthesis (BBN) constraints derived from the primordial Helium and Deuterium abundances [4], indicate that the number of effective relativistic species is N eff = 3.56 ± 0.23.…”

Section: Introductionmentioning

confidence: 99%

“…While theoretical biases have served as a guide for searches and model-building, in principle, very little is known about its nature and properties. Specifically, the DM mass can span the range 10 −15 -10 15 GeV, and its interaction cross-section with nucleons and annihilation cross-section into SM particles can lie in the range 10 −76 -10 −41 cm 2 [1].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The direct detection of boosted dark matter at high energies and PeV events at IceCube

Bhattacharya

Gandhi

Gupta

2015

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract. We study the possibility of detecting dark matter directly via a small but energetic component that is allowed within present-day constraints. Drawing closely upon the fact that neutral current neutrino nucleon interactions are indistinguishable from DM-nucleon interactions at low energies, we extend this feature to high energies for a small, non-thermal but highly energetic population of DM particle χ, created via the decay of a significantly more massive and long-lived non-thermal relic φ, which forms the bulk of DM. If χ interacts with nucleons, its cross-section, like the neutrino-nucleus coherent cross-section, can rise sharply with energy leading to deep inelastic scattering, similar to neutral current neutrino-nucleon interactions at high energies. Thus, its direct detection may be possible via cascades in very large neutrino detectors. As a specific example, we apply this notion to the recently reported three ultra-high energy PeV cascade events clustered around 1 − 2 PeV at IceCube (IC). We discuss the features which may help discriminate this scenario from one in which only astrophysical neutrinos constitute the event sample in detectors like IC.

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The direct detection of boosted dark matter at high energies and PeV events at IceCube

Bhattacharya

Gandhi

Gupta

2015

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…Taking into account that Kurie plots often deviate from linearity due to energy losses of low energy β-particles, he found a possible admixture ≤ 0.1 for 0.1 keV ≤ m i ≤ 3 MeV. Schreckenbach et al [186] searched for an admixture of sterile neutrinos in the β-decay of 64 Cu (T 1/2 = 12.7 h) that proceeds via β + and βbranches with endpoint energies of = 653 keV and = 579 keV, respectively. The 64 Cu activity of 3.3·10 11 Bq was produced by (n, γ) reaction in a thermal neutron flux of 3·10 14 cm -2 s -1 .…”

Section: Previous Experimentsmentioning

confidence: 99%

“…Best upper limits on the admixture |U e4 | 2 of sterile neutrinos derived from measured β-ray spectra. All upper limits refer to the 95 % CL except those for 64…”

Section: Previous Experimentsmentioning

confidence: 99%

Constraints on the Active and Sterile Neutrino Masses from Beta-Ray Spectra: Past, Present and Future1

Dragoun¹,

Vénos²

2016

PHY

View full text Add to dashboard Cite

Abstract:Although neutrinos are probably the most abundant fermions of the universe their mass is not yet known. Oscillation experiments have proven that at least one of the neutrino mass states has m i > 0.05 eV while various interpretations of cosmological observations yielded an upper limit for the sum of neutrino masses ∑m i < (0.14 -1.7) eV. The searches for the yet unobserved 0νββ decay result in an effective neutrino mass m ββ < (0.2 -0.7) eV. The analyses of measured tritium β-spectra provide an upper limit for the effective electron neutrino mass m(v e ) < 2 eV. In this review, we summarize the experience of two generations of β-ray spectroscopists who improved the upper limit of m(v e ) by three orders of magnitude. We describe important steps in the development of radioactive sources and electron spectrometers, and recapitulate the lessons from now-disproved claims for the neutrino mass of 30 eV and the 17 keV neutrino with an admixture larger than 0.03%. We also pay attention to new experimental approaches and searches for hypothetical sterile neutrinos.

show abstract

Calculation of momentum distribution function of a non-thermal fermionic dark matter

Biswas

Gupta

2017

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

The most widely studied scenario in dark matter phenomenology is the thermal WIMP scenario. Inspite of numerous efforts to detect WIMP, till now we have no direct evidence for it. A possible explanation for this non-observation of dark matter could be because of its very feeble interaction strength and hence, failing to thermalise with the rest of the cosmic soup. In other words, the dark matter might be of non-thermal origin where the relic density is obtained by the so-called freeze-in mechanism. Furthermore, if this non-thermal dark matter is itself produced substantially from the decay of another non-thermal mother particle, then their distribution functions may differ in both size and shape from the usual equilibrium distribution function. In this work, we have studied such a non-thermal (fermionic) dark matter scenario in the light of a new type of U(1) B−L model. The U(1) B−L model is interesting, since, besides being anomaly free, it can give rise to neutrino mass by Type II see-saw mechanism. Moreover, as we will show, it can accommodate a non-thermal fermionic dark matter as well. Starting from the collision terms, we have calculated the momentum distribution function for the dark matter by solving a coupled system of Boltzmann equations. We then used it to calculate the final relic abundance, as well as other relevant physical quantities. We have also compared our result with that obtained from solving the usual Boltzmann (or rate) equations directly in terms of comoving number density, Y . Our findings suggest that the latter approximation is valid only in cases where the system under study is close to equilibrium, and hence should be used with caution.

show abstract

Neutrinos and dark matter

Cited by 5 publications

References 38 publications

The direct detection of boosted dark matter at high energies and PeV events at IceCube

The direct detection of boosted dark matter at high energies and PeV events at IceCube

Constraints on the Active and Sterile Neutrino Masses from Beta-Ray Spectra: Past, Present and Future1

Calculation of momentum distribution function of a non-thermal fermionic dark matter

Contact Info

Product

Resources

About