Erratum: Review of Particle Properties

Hikasa, K.; Hagiwara, K.; Kawabata, S.; Barnett, R. M.; Groom, D. E.; Trippe, TG; Wohl, C.G.; Yost, G.P.; Armstrong, B.; Wagman, G.S.; Stone, James L.; Porter, F. C.; Morrison, R. J.; Cutkosky, R. E.; Montanet, L.; Gieselmann, K.; Aguilar-Benı́tez, M.; Caso, C.; Crawford, Ronald L.; Roos, M.; Törnqvist, Nils A.; Hayes, K.; Höhler, G.; Manley, D. M.; Olive, Keith A.; Shrock, Robert; Eidelman, S.; Schindler, R. H.; Hernández, J. J.; Conforto, G.; Eichler, R.

doi:10.1103/physrevd.46.5210

Cited by 73 publications

(81 citation statements)

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“…II. In what follows, I shall use the prescription of the Particle Data Group [36] for estimating confidence limits, namely, I shall assume that the errors shown in Eq. (14) are normally distributed with a mean value at −0.004 but with a renormalized probability distribution that is non-zero only when the manifestly positive quantity between the brackets in Eq.…”

Section: E Constraint On Excited State Transitionsmentioning

confidence: 99%

Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

1997

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Neutrino absorption cross sections for 71 Ga are calculated for all solar neutrino sources with standard energy spectra, and for laboratory sources of 51 Cr and 37 Ar; the calculations include, where appropriate, the thermal energy of decaying solar ions and use improved nuclear and atomic data. The ratio, R, of measured (in GALLEX and SAGE) to calculated 51 Cr capture rate is R = 0.95±0.07 (exp) + +0.04 −0.03 (theory). Cross sections are also calculated for specific neutrino energies chosen so that a spline fit determines accurately the event rates in a gallium detector even if new physics changes the energy spectrum of solar neutrinos. Theoretical uncertainties are estimated for cross sections at specific energies and for standard neutrino energy spectra. Standard energy spectra are presented for pp and CNO neutrino sources in the appendices. Neutrino fluxes predicted by standard solar models, corrected for diffusion, have been in the range 120 SNU to 141 SNU since 1968.Typeset using REVT E X

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Section: E Constraint On Excited State Transitionsmentioning

confidence: 99%

Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

1997

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“…Hence, pair production has only a small effect on P (r, E; E c ) for E c ≥ 10 20 eV, where the proton life time due to pion production is ≤ 3 × 10 8 yr. We calculated therefore P (r, E; E c ) taking into account pion production interactions only. We used the compilation of cross sections given in Hikasa et al (1992), and assumed that the total cross section corresponds to the isotropic production of a single pion (this assumption has been shown to be adequate in Yoshida & Teshima 1993;Aharonian & Cronin 1994). The resulting probability distribution may be approximated well over the energy range of interest by a function of the form…”

Section: Resultsmentioning

confidence: 99%

Ultra–High‐Energy Cosmic Rays May Come from Clustered Sources

Bahcall

Waxman

2000

ApJ

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Clustering of cosmic-ray sources affects the flux observed beyond the cutoff imposed by the cosmic microwave background and may be important in interpreting the AGASA, Fly's Eye, and HiRes data. The standard deviation, σ, in the predicted number, N , of events above 10 20 eV is σ/N = 0.9(r 0 /10 Mpc) 0.9 , where r 0 is the unknown scale length of the correlation function (r 0 ≃ 10 Mpc for field galaxies, H 0 = 50 km s −1 Mpc −1 ). Future experiments will allow the determination of r 0 through the detection of anisotropies in arrival directions of ∼ 10 20 eV cosmic-rays over angular scales of Θ ∼ r 0 /30 Mpc.

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“…Mixing in the quark sector is described by the Cabbibo-Kobayashi-Maskawa (3×3) unitary matrix V ij . It is known to a rather high accuracy [1], and the information about mixing parameters is continually refined. It is natural to expect that a similar mixing phenomenon occurs in the lepton sector of the SM as well, provided that the neutrino mass spectrum is nondegenerate.…”

Section: Introductionmentioning

confidence: 99%

“…It was shown in [9] that a new type of mixing -mixing in quark-lepton currents -must be considered in this approach. The resulting additional freedom in the choice of parameters makes it possible to remove the lower bound on the vector-leptoquark mass M X obtained from rare decays of π and K mesons [1]. The only constraint that does not depend on mixing arises from the cosmological estimate of the width of the decay π 0 → νν [10]: M X > 18 eV.…”

Section: Introductionmentioning

confidence: 99%

Neutrino radiative decay in an external electromagnetic field via vector leptoquark

1997

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The massive neutrino radiative decay ν i → ν j γ (i = j) is investigated within the Minimal Quark-Lepton Symmetry of the Pati-Salam type based on the SU (4) V ×SU (2) L ×G R group in an external constant crossed field ( E ⊥ H, E = H). The matrix element ∆M (X) and the decay probability W (X) due to the leptoquark X contribution are analysed. The effect of significant enhancement of the neutrino decay by the crossed field takes place. It is shown that the leptoquark contribution to the decay probability can dominate over the W -boson one in the case of strong suppression of the lepton mixing in the framework of the SM.To be published in Physics Letters B

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Erratum: Review of Particle Properties

Abstract: ERRATA v @,=arg(g,,g~, I = @ + ---m o d r 2 (instead of @+ -modv).As a consequence, the CP-violating asymmetry given by Eq. i26), is ( 14.331 1.3 )%, significantly larger than the result i 3.8+ 1.4 1% stated in the paper.

Cited by 73 publications

References 0 publications

Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

Ultra–High‐Energy Cosmic Rays May Come from Clustered Sources

Neutrino radiative decay in an external electromagnetic field via vector leptoquark

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