The sensitivity of a large water Čerenkov neutrino telescope in detecting possible oscillations (v μ→v τ) and (v μ→v e) of atmospheric neutrinos is studied, taking also into account the Wolfenstein, Mikheyev and Smirnov matter effects. The large water Čerenkov device is able to detect with high accuracy upward-going muons with energies greater than 10 GeV. After one year running time the search for ν oscillations will reach the following sensitivity for the oscillation parameters: Δm 2>3·10−3 (eV2), for sin22θ=1, sin22θ>4·10−2, for Δm 2>0.1 (eV2) for the oscillation (v μ→v τ) and δm 2>4·10−3 (eV2), for sin22θ=1, sin22θ>8·10−3, for δm 2=6·10−2 (eV2) for the oscillation (v μ→v e). These limits are well below the current accelerator and reactor limits. It is also stressed the importance of such a measurement in the context of solar ν puzzle.

OSCILLATIONS OF ATMOSPHERIC NEUTRINOS WITH A LARGE NEUTRINO TELESCOPE

LAVEDER, MARCO
1990

Abstract

The sensitivity of a large water Čerenkov neutrino telescope in detecting possible oscillations (v μ→v τ) and (v μ→v e) of atmospheric neutrinos is studied, taking also into account the Wolfenstein, Mikheyev and Smirnov matter effects. The large water Čerenkov device is able to detect with high accuracy upward-going muons with energies greater than 10 GeV. After one year running time the search for ν oscillations will reach the following sensitivity for the oscillation parameters: Δm 2>3·10−3 (eV2), for sin22θ=1, sin22θ>4·10−2, for Δm 2>0.1 (eV2) for the oscillation (v μ→v τ) and δm 2>4·10−3 (eV2), for sin22θ=1, sin22θ>8·10−3, for δm 2=6·10−2 (eV2) for the oscillation (v μ→v e). These limits are well below the current accelerator and reactor limits. It is also stressed the importance of such a measurement in the context of solar ν puzzle.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11577/121445
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