We further develop a recently proposed new approach to the description of the relativistic neutrino flavour ν L e ↔ ν L µ , spin ν L e ↔ ν R e and spin-flavour ν L e ↔ ν R µ oscillations in a constant magnetic field that is based on the use of the exact neutrino stationary states in the magnetic field. The neutrino flavour, spin and spin-flavour oscillations probabilities are calculated accounting for the whole set of possible conversions between four neutrino states. In general, the obtained expressions for the neutrino oscillations probabilities exhibit new inherent features in the oscillation patterns. It is shown, in particular, that: 1) in the presence of the transversal magnetic field for a given choice of parameters (the energy and magnetic moments of neutrinos and the strength of the magnetic field) the amplitude of the flavour oscillations ν L e ↔ ν L µ at the vacuum frequency is modulated by the magnetic field frequency, 2) the neutrino spin oscillation probability (without change of the neutrino flavour) exhibits the dependence on the mass square difference ∆m 2 . CONTENTS

Erratum: Measurement of the J/ψ pair production cross-section in pp collisions at √ s = 13 TeVThe LHCb collaboration E-mail: liupan.an@cern.ch Erratum to: JHEP06(2017)047ArXiv ePrint: 1612.07451The measurement of the differential cross-section as a function of p T (J/ψ J/ψ ) was incorrectly reported in the paper [1], due to an incorrect propagation of the efficiency values in the final analysis. In this erratum, all tables and figures that need to be corrected are reported, with identical numbering and captions to those in the orginial paper. In figure 2, only the data points are changed. In figure 9, the results of templated double parton scattering (DPS) fit for dσ(J/ψ J/ψ ) dp T (J/ψ J/ψ ) (the left column) are changed. In table 3, the percentages of the DPS component determined with p T (J/ψ J/ψ ) (the first row) are changed. In table 4, the σ eff values from the DPS fits for p T (J/ψ J/ψ ) (the first row) are changed. As a result, the values of σ eff for the models considered in the analysis are between 8.8 and 12.5 mb, instead of 10.0 and 12.5 mb. None of these changes affect the interpretation of the results and the conclusions.

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In this paper we considered semiclassical neutrino spin precession in a transversal matter current and quantum case of the neutrino spin oscillations in the mass and flavor bases induced by a moving media. In the first part we have verified, that even without presence of an electromagnetic field, in presence of a matter, when the transverse matter term is not zero, the neutrino spin oscillations can be induced. In the second part there were some calculations, that in the end led us to the evolution equations which include an effective Hamiltonian of the weak interactions. From these equations one can see the influence of the transverse component of a matter velocity on a spin oscillations and of the longitudinal component of a matter velocity on the neutrino energy spectrum.

We adopt the approach to the problem of neutrino oscillations in a magnetic field introduced in [1] and extended to the case of three neutrino generations in [2] to investigate the impact of ultrahighenergy neutrino oscillations in the interstellar magnetic field. Based on the assumption that UHE neutrinos flavour distribution follows the pattern 1:2:0, we have estimated the fluxes detected by a terrestrial neutrino telescope. We find out that the interaction with a magnetic field does not significantly modify the flavour distribution of UHE neutrinos unless they possess transition magnetic moments.