Measurement of the total active 8B solar neutrino flux at the Sudbury Neutrino Observatory with enhanced neutral current sensitivity
Physical Review Letters 92 (2004) article 181301 6 pages
Constraints on Nucleon Decay via Invisible Modes from the Sudbury Neutrino Observatory
Physical Review Letters 92 (2004) 102004 4pp
Electron antineutrino search at the Sudbury Neutrino Observatory
Physical Review D - Particles, Fields, Gravitation and Cosmology 70:9 (2004)
Abstract:
Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained. © 2004 The American Physical Society.A search for correlations of TeV gamma rays with ultra-high-energy cosmic rays
Astrophysical Journal 586:2 I (2003) 1232-1237
Abstract:
A search was conducted for TeV γ-rays emitted from the direction of the ultra-high-energy cosmic ray detected by the Fly's Eye experiment with energy E ∼ 3 × 1020 eV. No enhancement was found at a level of 10-10 cm-2 s-1 for E > 350 GeV. A steady source of ultra-high-energy cosmic ray protons or photons would be expected to produce a γ-ray flux above this level. An upper limit was also set for the flux of TeV γ-rays from 3C 147, the most prominent active galactic nucleus in the error box.Neutral current and day night measurements from the pure D2O phase of SNO
Nuclear and Particle Physics Proceedings Elsevier 118 (2003) 3-14