Table 1
Major neutrino reactions.
| Reaction | # Targets | # Signal hits | Signal fraction | Reference |
|
|
||||
|
6 × 1037 | 134 k (157 k) | 93.8% (94.4%) | Strumia & Vissani (2003) |
| νe + e− → νe + e − | 3 × 1038 | 2.35 k (2.25 k) | 1.7% (1.4%) | Marciano & Parsa (2003) |
|
3 × 1038 | 660 (720) | 0.5% (0.4%) | Marciano & Parsa (2003) |
| νμ + τ + e− → νμ + τ + e − | 3 × 1038 | 700 (720) | 0.5% (0.4%) | Marciano & Parsa (2003) |
|
3 × 1038 | 600 (570) | 0.4% (0.4%) | Marciano & Parsa (2003) |
| νe + 16O → e − + X | 3 × 1037 | 2.15 k (1.50 k) | 1.5% (0.9%) | Kolbe et al. (2002) |
|
3 × 1037 | 1.90 k (2.80 k) | 1.3% (1.7%) | Kolbe et al. (2002) |
| νall + 16O → νall + X | 3 × 1037 | 430 (410) | 0.3% (0.3%) | Kolbe et al. (2002) |
|
6 × 1034 | 270 (245) | 0.2% (0.2%) | Haxton (1999) |
Notes. The approximate number of targets in a 1 km3 ice detector, the detected number of hits at 10 kpc distance and their fraction in stars are given in the second, third and fourth column, respectively. In order to indicate the effect of neutrino oscillations in the star, signal hits and fractions are presented both assuming a normal neutrino hierarchy (Scenario A) and – in brackets – assuming an inverted hierarchy (Scenario B). The numbers are taken from the Garching model using the equation of state by Lattimer & Swesty (1991), integrating over 0.8 s and averaging over the neutrino incidence angle.
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