Prediction of neutrino fluxes in the NOMAD experiment
✍ Scribed by P Astier; D Autiero; A Baldisseri; M Baldo-Ceolin; M Banner; G Bassompierre; K Benslama; N Besson; I Bird; B Blumenfeld; F Bobisut; J Bouchez; S Boyd; A Bueno; S Bunyatov; L Camilleri; A Cardini; P.W Cattaneo; V Cavasinni; A Cervera-Villanueva; G Collazuol; G Conforto; C Conta; R Cousins; D Daniels; H Degaudenzi; T Del Prete; A De Santo; T Dignan; L Di Lella; E do Couto e Silva; J Dumarchez; M Ellis; G.J Feldman; A Ferrari; R Ferrari; D Ferrère; V Flaminio; M Fraternali; J.-M Gaillard; E Gangler; A Geiser; D Geppert; D Gibin; S Gninenko; A Godley; J.-J Gomez-Cadenas; J Gosset; C Gößling; M Gouanère; A Grant; G Graziani; A Guglielmi; C Hagner; J Hernando; T.M Hong; D Hubbard; P Hurst; N Hyett; E Iacopini; C Joseph; F Juget; M Kirsanov; O Klimov; J Kokkonen; A Kovzelev; A Krasnoperov; C Lachaud; B Lakić; A Lanza; L La Rotonda; M Laveder; A Letessier-Selvon; J.-M Levy; L Linssen; A Ljubičić; J Long; A Lupi; A Marchionni; F Martelli; X Méchain; J.-P Mendiburu; J.-P Meyer; M Mezzetto; S.R Mishra; G.F Moorhead; P Nédélec; Yu Nefedov; C Nguyen-Mau; D Orestano; F Pastore; L.S Peak; E Pennacchio; H Pessard; R Petti; A Placci; G Polesello; D Pollmann; A Polyarush; B Popov; C Poulsen; J Rico; P Riemann; C Roda; A Rubbia; F Salvatore; K Schahmaneche; B Schmidt; T Schmidt; M Sevior; D Shih; D Sillou; F.J.P Soler; G Sozzi; D Steele; U Stiegler; M Stipčević; Th Stolarczyk; M Tareb-Reyes; G.N Taylor; V Tereshchenko; A Toropin; A.-M Touchard; S.N Tovey; M.-T Tran; E Tsesmelis; J Ulrichs; L Vacavant; M Valdata-Nappi; V Valuev; F Vannucci; K.E Varvell; M Veltri; V Vercesi; G Vidal-Sitjes; J.-M Vieira; T Vinogradova; F.V Weber; T Weisse; F.F Wilson; L.J Winton; B.D Yabsley; H Zaccone; K Zuber
- Publisher
- Elsevier Science
- Year
- 2003
- Tongue
- English
- Weight
- 547 KB
- Volume
- 515
- Category
- Article
- ISSN
- 0168-9002
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📜 SIMILAR VOLUMES
The uncertainty in the calculation of atmospheric neutrino fluxes is studied. The absolute value of atmospheric neutrino fluxes is sensitive to variation of the primary cosmic ray flux model asld/or the interaction model. However, the ratios between different kind of neutrinos stay almost unchanged