The Role of tau-neutrino ultrahigh-energy astrophysics in km**3 detectors

Feb, 1997
14 pages
e-Print:
Report number:
  • INFN-1166-97,
  • ROMAI-17-2-97,
  • EE-PUP-1074

Citations per year

1997200320092015201902468
Abstract: (arXiv)
We show that the expected ντ \nu_{\tau} signals, by their secondary tau tracks, in Km^3 detectors at highest cosmic ray energy window 1.71021eV>Eτ>1.6x1017eV 1.7\cdot 10^{21} eV \gt E_{\tau} \gt 1.6 x 10^{17} eV, must overcome the corresponding νμ \nu_{\mu} (or muonic) ones. Indeed, the Lorentz-boosted tau range length grows (linearly) above muon range, for E_{\tau} \RAISE 1.6 x 10^8 GeV and reaches its maxima extension, Rτmax191km R_{\tau_{\max}} \simeq 191 km, at energy Eτ3.8x109GeVE_{\tau} \simeq 3.8 x 10^9 GeV. At this peak the tau range is nearly 20 times the corresponding muon range (at the same energy) implying a similar ratio in ντ \nu_{\tau} over νμ \nu_{\mu} detectability. This dominance, however may lead (at present most abundant ντ \nu_{\tau} model fluxes) to just a rare spectacular event a year (if flavor mixing occurs). Lower energetic τ \tau and ντ \nu_{\tau} signals (νˉeeνˉττ,ντN...) (\bar{\nu}_e e\to \bar{\nu}_{\tau} \tau, \nu_{\tau} N\to ...) at energy range (105÷107GeV 10^5 \div 10^7 GeV) may be more easily observed in km^3 detectors at a rate of a few (νˉeeνˉττ) (\bar{\nu}_e e\to \bar{\nu}_{\tau} \tau) to tens event (ντNτ+ (\nu_{\tau} N\to \tau + anything) a year.
  • neutrino/tau: search for
  • neutrino/tau: particle source
  • astrophysics
  • neutrino nucleon: interaction
  • tau: neutrinoproduction
  • tau: path length
  • muon: path length
  • energy dependence
  • antineutrino electron: interaction
  • antineutrino/e