The role of ν_τ ultrahigh energy astrophysics in Km^3 detectors
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arXiv
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| Formato: | Preprint |
| Publicado: |
1997
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| _version_ | 1866917292848185344 |
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| author | Fargion, D. |
| author_facet | Fargion, D. |
| contents | We show that the expected $ ν_τ $ signals, by their secondary tau tracks, in Km^3 detectors at highest cosmic ray energy window $ 1.7\cdot 10^{21} eV \gt E_τ \gt 1.6 x 10^{17} eV$, must overcome the corresponding $ ν_μ $ (or muonic) ones. Indeed, the Lorentz-boosted tau range length grows (linearly) above muon range, for $ E_τ \RAISE 1.6 x 10^8 GeV$ and reaches its maxima extension, $ R_{τ_{\max}} \simeq 191 km$, at energy $E_τ \simeq 3.8 x 10^9 GeV$. At this peak the tau range is nearly 20 times the corresponding muon range (at the same energy) implying a similar ratio in $ ν_τ $ over $ ν_μ $ detectability. This dominance, however may lead (at present most abundant $ ν_τ $ model fluxes) to just a rare spectacular event a year (if flavor mixing occurs). Lower energetic $ τ$ and $ ν_τ $ signals $ (\barν_e e\to \barν_τ τ, ν_τ N\to ...) $ at energy range ($ 10^5 ÷10^7 GeV$) may be more easily observed in km^3 detectors at a rate of a few $ (\barν_e e\to \barν_τ τ) $ to tens event $ (ν_τ N\to τ+ $ anything) a year. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_astro_ph_9704205 |
| institution | arXiv |
| publishDate | 1997 |
| record_format | arxiv |
| spellingShingle | The role of ν_τ ultrahigh energy astrophysics in Km^3 detectors Fargion, D. Astrophysics High Energy Astrophysical Phenomena High Energy Physics - Phenomenology Nuclear Experiment Nuclear Theory We show that the expected $ ν_τ $ signals, by their secondary tau tracks, in Km^3 detectors at highest cosmic ray energy window $ 1.7\cdot 10^{21} eV \gt E_τ \gt 1.6 x 10^{17} eV$, must overcome the corresponding $ ν_μ $ (or muonic) ones. Indeed, the Lorentz-boosted tau range length grows (linearly) above muon range, for $ E_τ \RAISE 1.6 x 10^8 GeV$ and reaches its maxima extension, $ R_{τ_{\max}} \simeq 191 km$, at energy $E_τ \simeq 3.8 x 10^9 GeV$. At this peak the tau range is nearly 20 times the corresponding muon range (at the same energy) implying a similar ratio in $ ν_τ $ over $ ν_μ $ detectability. This dominance, however may lead (at present most abundant $ ν_τ $ model fluxes) to just a rare spectacular event a year (if flavor mixing occurs). Lower energetic $ τ$ and $ ν_τ $ signals $ (\barν_e e\to \barν_τ τ, ν_τ N\to ...) $ at energy range ($ 10^5 ÷10^7 GeV$) may be more easily observed in km^3 detectors at a rate of a few $ (\barν_e e\to \barν_τ τ) $ to tens event $ (ν_τ N\to τ+ $ anything) a year. |
| title | The role of ν_τ ultrahigh energy astrophysics in Km^3 detectors |
| topic | Astrophysics High Energy Astrophysical Phenomena High Energy Physics - Phenomenology Nuclear Experiment Nuclear Theory |
| url | https://arxiv.org/abs/astro-ph/9704205 |