Lightest Nuclei in UHECR versus Tau Neutrino Astronomy

UHECR may be either nucleons [Abraham J. et al., (Pierre Auger Collaboration), Science, vol.318, p.939-943 (arXiv:0711.2256)] or nuclei; in the latter case the Lightest Nuclei, as He4 or He3, Li, Be, explains at best the absence of Virgo signals and the crowding of events around Cen-A bent by galactic magnetic fields [Fargion D., Phys. Scr. 78 (2008) 045901, 1-4]. This model fit the observed nuclear mass composition discovered in AUGER. However UHECR nucleons above GZK produce EeV neutrinos while Heavy Nuclei, as Fe UHECR do not produce much. UHECR He nuclei at few 1019eV suffer nuclear fragmentation (producing low energetic neutrino at tens PeVs) but it suffer anyway photo-pion GZK suppression (leading to EeV neutrinos) once above one-few 1020eV. Both these cosmogenic UHE secondary neutrinos signals may influence usual predicted GZK [Greisen K., 1966 Phys. Rev. Lett. 16 748], [Zatsepin, G.T., Kuz'min, V.A., Zh. Eks. Teor. Fiz., Pis'ma Red.4 (1966) 144] Tau Neutrino Astronomy [D. Fargion, et al.: “Horizontal Tau air showers from mountains in deep valley. Traces of UHECR neutrino tau” 26th ICRC, He 6.1.09, p.396-398. 1999. (USA); Fargion D., 2002, ApJ, 570, 909; Fargion D. et al. 1999, 26th ICRC, HE6.1.10, 396-398; Fargion D., et al. 2004, ApJ, 613, 1285; Fargion D. et al., Nuclear Physics B (Proc. Suppl.) 2004; Fargion D., et al. Adv. in Space Res., 37 (2006) 2132-2138; 136, 119; D. Fargion, J. Phys. Soc. Jpn. Vol.77 (2008) Suppl. B., p.1-15; Fargion D. et al. Adv. Space Res. 37 (2006) 2132-2138] in significant and detectable way; the role of resonant antineutrino electron-electron leading to Tau air-shower may also rise.