Triangle inequalities for Majorana-neutrino magnetic moments

Frère, Jean‐Marie; Heeck, Julian; Mollet, Simon

doi:10.1103/physrevd.92.053002

Cited by 10 publications

(13 citation statements)

References 17 publications

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“…2 [for analytic expressions, see Eqs. (21) and (22)] could be used to determine the nature of neutrinos. If the parameters measured in neutrino scattering experiments are out of the Majorana bound but inside the Dirac bound, then neutrinos are Dirac particles.…”

Section: Discussionmentioning

confidence: 99%

“…Here we shall analytically derive the Dirac bound (21) and the Majorana bound (22). In the Dirac case, we write (A, B, C) in the following form…”

Section: Appendix: Proofmentioning

confidence: 99%

“…(A.9), the side lengths of the parallelogram should be L + and L − . If one angle of the parallelogram is defined as α, then we have the following transformation from (L + , L − , α) to (G, H, γ): Then by converting (A, B, C) to (X, Y ), it is straightforward to get the Majorana bound (22).…”

Section: Appendix: Proofmentioning

confidence: 99%

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Distinguishing between Dirac and Majorana neutrinos in the presence of general interactions

Rodejohann

Yaguna

2017

J. High Energ. Phys.

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Abstract:We revisit the possibility of distinguishing between Dirac and Majorana neutrinos via neutrino-electron elastic scattering in the presence of all possible Lorentz-invariant interactions. Defining proper observables, certain regions of the parameter space can only be reached for Dirac neutrinos, but never for Majorana neutrinos, thus providing an alternative method to differentiate these two possibilities. We first derive analytically and numerically the most general conditions that would allow to distinguish Dirac from Majorana neutrinos, both in the relativistic and non-relativistic cases. Then, we apply these conditions to data on ν µ -e andν e -e scatterings, from the CHARM-II and TEXONO experiments, and find that they are consistent with both types of neutrinos. Finally, we comment on future prospects of this kind of tests.

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Section: Discussionmentioning

confidence: 99%

“…Here we shall analytically derive the Dirac bound (21) and the Majorana bound (22). In the Dirac case, we write (A, B, C) in the following form…”

Section: Appendix: Proofmentioning

confidence: 99%

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Distinguishing between Dirac and Majorana neutrinos in the presence of general interactions

Rodejohann

Yaguna

2017

J. High Energ. Phys.

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“…It is also useful to note that the effective Majorana moments defined in Eq. (III.5) have recently been shown to fulfill the triangle inequality µ 2 τ,eff ≤ µ 2 e,eff + µ 2 µ,eff [45], although we do not make use of this property here since primordial abundances are found as a function of transition moments. electron and mu/tau neutrinos as a function of effective magnetic moment.…”

Section: Decoupling Temperature and Interaction Rate Calculationmentioning

confidence: 99%

Majorana neutrino magnetic moment and neutrino decoupling in big bang nucleosynthesis

et al. 2015

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We examine the physics of the early universe when Majorana neutrinos (νe, νµ, ντ ) possess transition magnetic moments. These extra couplings beyond the usual weak interaction couplings alter the way neutrinos decouple from the plasma of electrons/positrons and photons. We calculate how transition magnetic moment couplings modify neutrino decoupling temperatures, and then use a full weak, strong, and electromagnetic reaction network to compute corresponding changes in Big Bang Nucleosynthesis abundance yields. We find that light element abundances and other cosmological parameters are sensitive to magnetic couplings on the order of 10 −10 µB. Given the recent analysis of sub-MeV Borexino data which constrains Majorana moments to the order of 10 −11 µB or less, we find that changes in cosmological parameters from magnetic contributions to neutrino decoupling temperatures are below the level of upcoming precision observations.

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“…[15,16] for a thorough review). However, new physics contributions could enhance the predicted magnetic moment [17][18][19][20][21][22][23][24]. In particular, Ref.…”

Section: Introductionmentioning

confidence: 99%

Precision constraints on radiative neutrino decay with CMB spectral distortion

et al. 2018

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We investigate the radiative decay of the cosmic neutrino background, and its impact on the spectrum of the cosmic microwave background (CMB) that is known to be a nearly perfect black body. We derive exact formulae for the decay of a heavier neutrino into a lighter neutrino and a photon, νj → νi + γ, and of absorption as its inverse, νi + γ → νj, by accounting for the precise form of the neutrino momentum distribution. Our calculations show that if the neutrinos are heavier than O(0.1) eV, the exact formulae give results that differ by ∼50%, compared with approximate ones where neutrinos are assumed to be at rest. We also find that spectral distortion due to absorption is more important for heavy neutrino masses (by a factor of ∼10 going from a neutrino mass of 0.01 eV to 0.1 eV). By analyzing the CMB spectral data measured with COBE-FIRAS, we obtain lower limits on the neutrino lifetime of τ12 4 × 10 21 s (95% C.L.) for the smaller mass splitting and τ13 ∼ τ23 10 19 s for the larger mass splitting. These represent up to one order of magnitude improvement over previous CMB constraints. With future CMB experiments such as PIXIE, these limits will improve by roughly 4 orders of magnitude. This translates to a projected upper limit on the neutrino magnetic moment (for certain neutrino masses and decay modes) of µν < 3 × 10 −11 µB, where µB is the Bohr magneton. Such constraints would make future precision CMB measurements competitive with lab-based constraints on neutrino magnetic moments. PACS numbers: 13.35.Hb, 95.30.Cq, 98.70.Vc, 98.80.-k arXiv:1803.00588v2 [astro-ph.CO]

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Triangle inequalities for Majorana-neutrino magnetic moments

Cited by 10 publications

References 17 publications

Distinguishing between Dirac and Majorana neutrinos in the presence of general interactions

Distinguishing between Dirac and Majorana neutrinos in the presence of general interactions

Majorana neutrino magnetic moment and neutrino decoupling in big bang nucleosynthesis

Precision constraints on radiative neutrino decay with CMB spectral distortion

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