The MSW mechanism for three neutrino generations and the solar neutrino puzzle

We analyse the ³⁷Cl experiment for three neutrino generations with arbitrary mixing angles in the adiabatic approximation and present the resulting ⁸B-neutrino energy spectrum.     

Oscillations of three generations of neutrinos and the solar neutrino problem

The resonant neutrino oscillations in matter are assumed to be responsible for the observed reduction in the capture rate for the ³⁷Cl detector. The expression of the probability that a solar v_e reaches the Earth as a v_e is given in the case of three generations. In the small mixing angle approximation, we describe all the regions of neutrino parameters which give rise to a capture rate of 2.1 SNU for ³⁷Cl and we give the corresponding prediction for the ⁷¹Ga detector.     

Light pseudoscalar higgs and the number of generations

It is shown, within a two-Higgs doublet model, that the pseudoscalar Higgs particle P may be used as a counter of the total number of quark and lepton generations if it is light enough to be produced in the decay Z → Pγ. Numerical results are presented for this decay where the only known quantities are the number of generations and the ratio of vacuum expectation values for the neutral components of the two Higgs doublets.It is suggestedhow the latter quantity may be measured in other processes at the forthcoming e⁺e⁻ colliders, thus making an indirect measurement of the number of generations possible.     

Neutrino-pair bremsstrahlung and the number of lepton generations

Neutrino pair creation in bremsstrahlung processes of the type \(l \to l{\text{ }}v{\text{ }}\bar v\) contains vital information on the number of lepton generations, and is catalyzed by the coherent nuclear Coulomb effect or other forms of intense fields. Of particular interest is the ratio \(R_{v\bar v} = \sigma [1\mathop \to \limits_A l(v\bar v)]/\sigma [1\mathop \to \limits_A l'(v\bar v)]\) (wherel, l′ are distinct charged leptons). It is sensitive to the number of neurino types and their couplings in the same way that the ratio \(R_{q\bar q} = \sigma [e^ + e^ - \to {\text{hadrons}}]/\sigma [e^ + e^ - \to \mu ^ + \mu ^ - ]\) is to those of quarks. In the Weinberg-Salam model withN lepton generations, the ratio \(R_{v\bar v}\) is approximately given by \([(N + 4) + 4(1 - 4\sin ^2 \theta _W )]/8\) .     

On the possible presence of neutral antileptons of all generations in the solar neutrino flux

The hypothesis that part of solar electron neutrino flux transforms into antineutrinos of the second and third generations and related antiparticles is considered. Complete electroweak spectra of recoil electrons, including impurity components, are obtained and analyzed for the scattering of beryllium monoenergetic solar neutrinos with energies of 0.862 MeV on an electron target.     

Photoproduction of neutrino pairs on an electron in a magnetic field

The spectral-angular and spectral distributions of the probability of photoproduction of neutrino pairs on an electron in a magnetic field are calculated. The dependence of the probability of this process on the magnetic-field strength, the orientation of the electron spin in the initial and final states, and also on the direction of the circular polarization of the wave is investigated.     

Production of neutrino pairs by an electron in a crossed field

It has been shown on a number of occasions [1, 2] that processes which are forbidden in the vacuum can occur in the presence of an external field. Of this kind is the process of production of neutrino pairs by an electron in an external field. It is well known that this process is forbidden in the vacuum, but the presence of the external field lifts the prohibition on this reaction. In itself, the production of neutrino pairs by an electron in an external field is of interest in connection with a number of questions in astrophysics such as, for example, energy loss by stars and the spectrum of cosmic-ray neutrinos. In addition, in connection with the indication [3] of the possible existence of neutral currents, we consider here the production of neutrino pairs by an electron in an external field in the low-energy approximation of the Weinberg-Salam model. The external field is taken to be a crossed field. This approximation of the external field is justified [4, 5] when one is considering the motion of a relativistic particle in almost any rapidly varying field.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 4, pp. 59–62, April, 1980.I thank A. A. Sokolov for interest in the work and A. V. Vorisov and V. Ch. Zhukovskii for discussing the results.     

Tiny neutrino mass from SUSY and lepton number breaking sector

We suggest a new setup where SUSY breaking spurion F-term possesses lepton number. This setup not only modifies sparticle mass spectra but also realizes several new models, where neutrino mass is naturally induced through radiative corrections. We here suggest two new models; the first one is (i): pseudo-Dirac/Schizophrenic neutrino model, and the second one is (ii): pure Majorana neutrino model. We will also show this setup can naturally apply to the supersymmetric Zee-Babu model.     

Observation of muon pairs in neutrino interactions at Serpukhov 70 GeV accelarator

A search for dimuons produced in a spark chamber experiment in neutrino and antineutrino beams of the Serpukhov accelerator is reported. The clear dimuon signal has been observed in vN interactions. R_v = N(2ω)/N(1ω)? (6.2 ± 1.7) × 10^?3 in the energy interval 7.5 ÷ 30 GeV. From antineutrino data we conclude that in the same energy range $\text{R}{}_{\mathrm{<mtext>v</mtext>}}\text{? 1.1. × 10}{}^{\mathrm{?2}}\text{(90\% C.L.)}$.     

Emission of neutrino pairs by an electron in an ultrastrong magnetic field

The transitions of relativistic electrons in a magnetic field with the emission of an antineutrino-neutrino pair are considered. Probabilities are obtained for electron transitions to the ground state and weakly excited states. It is shown that in the case of an ultrastrong magnetic field (HH_o=m²c³/e=4.41·10¹³ G) such transitions made a considerable contribution to the total probability of the process.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 3, pp. 110–114, March, 1978.In conclusion, the authors express their profound gratitude to A. A. Sokolov for his attention to our work.     

Mean square number fluctuation for a fermion source and its dependence on neutrino mass for the universal cosmic neutrino background

Using the general formulation for obtaining chemical potentialμ of an ideal Fermi gas of particles at temperature T, with particle rest mass m₀ and average density 〈N〉/V, the dependence of the mean square number fluctuation 〈ΔN ²〉/V on the particle mass m₀ has been calculated explicitly. The numerical calculations are exact in all cases whether rest mass energym ₀c² is very large (non-relativistic case), very small (ultra-relativistic case) or of the same order as the thermal energy k_BT. Application of our results to the detection of the universal very low energy cosmic neutrino background (CNB), from any of the three species of neutrinos, shows that it is possible to estimate the neutrino mass of these species if from approximate experimental measurements of their momentum distribution one can extract, someday, not only the density 〈N _v〉/V but also the mean square fluctuation 〈Δ _v ² 〉/V. If at the present epoch, the universe is expanding much faster than thermalization rate for CNB, it is shown that our analysis leads to a scaled neutrino massm _v instead of the actual massm _0v .     

Resonant neutrino oscillations and the neutrino signature of supernovae

We examine the effects of resonant neutrino oscillations, proposed as a solution to the solar neutrino puzzle, on the neutrino signature of a Type II supernova. We find that, for parameters corresponding to an adiabatic conversion of most of the ⁸B neutrino flux, the supernova neutrino signal in a water-Čerenkov detector is altered in the following way: (1) The isotropic-to-directional event ratio increases; (2) The short time scale neutronization burst signal decreases by a factor 7, perhaps rendering it unobservable. Detection of these changes would allow one to distinguish between neutrino oscillations and solar model alterations as solutions to the solar neutrino problem. We also note that mixing of the higher energy ν_μ and ν_r's to ν_e's will enhance detection of the thermally produced ν-flux.     

Low Reynolds number hydrodynamics of asymmetric,oscillating dumbbell pairs

Numerical simulations are used to discuss various aspects of “optical rogue wave” statistics observed in noise-driven fiber supercontinuum generation associated with highly incoherent spectra. In particular, we consider how long wavelength spectral filtering influences the characteristics of the statistical distribution of peak power, and we contrast the statistics of the spectrally filtered SC with the statistics of both the peak power of the most red-shifted soliton in the SC and the maximum peak power across the full temporal field with no spectral selection. For the latter case, we show that the unfiltered statistical distribution can still exhibit a long-tail, but the extreme-events in this case correspond to collisions between solitons of different frequencies. These results confirm the importance of collision dynamics in supercontinuum generation. We also show that the collision-induced events satisfy an extended hydrodynamic definition of “rogue wave” characteristics.