ar X iv : 0 90 2 . 32 90 v 1 [ as tr o - ph . H E ] 1 9 Fe b 20 09 Lightest Nuclei in UHECR versus Tau Neutrino Astronomy

Abstract

UHECR may be either nucleons [2] or nuclei; in the latter case the Lightest Nuclei, as He or He, Li, Be , explains at best the absence of Virgo signals and the crowding of events around Cen-A bent by galactic magnetic fields [3]. 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 10eV 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 10eV . Both these cosmogenic UHE secondary neutrinos signals may influence usual predicted GZK [9],[12] Tau Neutrino Astronomy [4] in significant and detectable way; the role of resonant antineutrino electron-electron leading to Tau air-shower may also rise.

5 Figures and Tables

Cite this paper

@inproceedings{Fargion2009arXI, title={ar X iv : 0 90 2 . 32 90 v 1 [ as tr o - ph . H E ] 1 9 Fe b 20 09 Lightest Nuclei in UHECR versus Tau Neutrino Astronomy}, author={D . Fargion and Daniele D ’ Armiento and Paola Paggi and S . Patri}, year={2009} }