First observation of the neutral current nuclear excitation 12C(v,v′)12C∗(1+, 1)

Bodmann, B.; Booth, N. E.; Burtak, F.; Dodd, A.C.; Drexlin, G.; Eberhard, V.; Edgington, J.A.; Finckh, E.; Gemmeke, H.; Giorginis, G.; Glombik, A.; Gorringe, T. P.; Grandegger, W.; Hanika, T.; Kleifges, M.; Kleinfeller, J.; Kretschmer, W.; Malik, A.; Maschuw, R.; Meyer, R. A.; Plischke, P.; Raupp, F.; Schilling, F. P.; Seligmann, B.; Wochele, J.; Wolf, J.; Wölfle, S.; Zeitnitz, B.

doi:10.1016/0370-2693(91)90939-n

Cited by 70 publications

(9 citation statements)

References 10 publications

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“…A fit to the e + events between 20 and 60 MeV yields a total excess of 51.8 +18. 7 −16.9 ± 8.0 events. If attributed toνµ →νe oscillations, this corresponds to an oscillation probability of (0.31 +0.11 −0.10 ± 0.05)%.…”

mentioning

confidence: 98%

Evidence forν¯μ→ν¯eOscillation

Athanassopoulos¹,

Auerbach²,

Burman³

et al. 1996

Phys. Rev. Lett.

756

409

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A search forνµ →νe oscillations has been conducted at the Los Alamos Meson Physics Facility by usingνµ from µ + decay at rest. Theνe are detected via the reactionνe p → e + n, correlated with a γ from np → dγ (2.2 MeV). The use of tight cuts to identify e + events with correlated γ rays yields 22 events with e + energy between 36 and 60 MeV and only 4.6 ± 0.6 background events. A fit to the e + events between 20 and 60 MeV yields a total excess of 51.8 +18.7 −16.9 ± 8.0 events. If attributed toνµ →νe oscillations, this corresponds to an oscillation probability of (0.31 +0.11 −0.10 ± 0.05)%. 14.60. Pq, 13.15.+g We present the results from a search for neutrino oscillations using the Liquid Scintillator Neutrino Detector (LSND) apparatus described in reference [1]. The existence of neutrino oscillations would imply that neutrinos have mass and that there is mixing among the different flavors of neutrinos. Candidate events in a search for the transformationν µ →ν e from neutrino oscillations with the LSND detector have previously been reported [2] for data taken in 1993 and 1994. Data taken in 1995 have been included in this paper, and the analysis has been made more efficient.Protons are accelerated by the LAMPF linac to 800 MeV kinetic energy and pass through a series of targets, culminating with the A6 beam stop. The primary neutrino flux comes from π + produced in a 30-cm-long water target in the A6 beam stop [1]. The total charge delivered to the beam stop while the detector recorded data was 1787 C in 1993, 5904 C in 1994, and 7081 C in 1995. Most of the π + come to rest and decay through the sequence π + → µ + ν µ , followed by µ + → e + ν eνµ , supplyingν µ with a maximum energy of 52.8 MeV. The energy dependence of theν µ flux from decay at rest (DAR) is very well known, and the absolute value is known to 7% [1,3]. The open space around the target is short compared to the pion decay length, so only 3% of the π + decay in flight (DIF). A much smaller fraction (approximately 0.001%) of the muons DIF, due to the difference in lifetimes and that a π + must first DIF. The totalν µ flux averaged over the detector volume, including contributions from upstream targets and all elements of the beam stop, was 7.6 × 10 −10ν µ /cm 2 /proton. Aν e component in the beam comes from the symmetrical decay chain starting with a π − . This background is suppressed by three factors in this experiment. First, π + production is about eight times the π − production in the beam stop. Second, 95% of π − will come to rest and are absorbed before decay in the beam stop. Third, 88% of µ − from π − DIF are captured from atomic orbit, a process which does not give aν e . Thus, the relative yield, compared to the positive channel, is estimated to be ∼ (1/8) × 0.05 × 0.12 = 7.5 × 10 −4 . A detailed Monte Carlo simulation [3], gives a value of 7.8 × 10 −4 for the flux ratio ofν e toν µ .The detector is a tank filled with 167 metric tons of dilute liquid scintillator, located about 30 m from the neutrino source, and surrounded on all s...

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mentioning

confidence: 98%

Evidence forν¯μ→ν¯eOscillation

Athanassopoulos¹,

Auerbach²,

Burman³

et al. 1996

Phys. Rev. Lett.

756

409

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“…The CCFR experiment [5] provides the most stringent limit on ν µ → ν e oscillations near ∆m 2 ∼ 350 eV 2 /c 4 , but their limits are not as restrictive as E776 for values of ∆m 2 < 300 eV 2 /c 4 . The KARMEN experiment [6] has searched for ν µ → ν e oscillations using neutrinos from pion DAR. These neutrinos are monoenergetic, and the signature for oscillations is an electron energy peak at about 12 MeV.…”

Section: B Comparison With Other Experimentsmentioning

confidence: 99%

Results onνμ→νeoscillations from pion decay in flight neutrinos

Athanassopoulos¹,

Auerbach²,

Burman³

et al. 1998

Phys. Rev. C

259

123

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A search for ν µ → ν e oscillations has been conducted at the Los Alamos Meson Physics Facility using ν µ from π + decay in flight. An excess in the number of beam-related events from the ν e C → e − X inclusive reaction is observed. The excess is too large to be explained by normal ν e contamination in the beam at a confidence level greater than 99%. If interpreted as an oscillation signal, the observed oscillation probability of (2.6±1.0±0.5)×10 −3 is consistent with the previously reportedν µ →ν e oscillation evidence from LSND.14.60.Pq, 13.15.+g Typeset using REVT E X 2

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“…12 C(ν e , e − ) 12 N and 12 C(ν, ν ′ ) 12 C * have also been performed at KARMEN [19], at LAMPF [20], and by LSND [21]. Table 2 compares the theoretical predictions to the measured data.…”

Section: Measurements Of Cross Sections Formentioning

confidence: 99%

Supernova neutrino detection in Borexino

Cadonati

Calaprice

Chen

2002

Astroparticle Physics

102

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We calculated the expected neutrino signal in Borexino from a typical Type II supernova at a distance of 10 kpc. A burst of around 110 events would appear in Borexino within a time interval of about 10 s. Most of these events would come from the reaction channelν e + p → e + + n, while about 30 events would be induced by the interaction of the supernova neutrino flux on 12 C in the liquid scintillator. Borexino can clearly distinguish between the neutral-current excitations 12 C(ν, ν ′ ) 12 C * (15.11 MeV) and the charged-current reactions 12 C(ν e , e − ) 12 N and 12 C(ν e , e + ) 12 B, via their distinctive event signatures. The ratio of the chargedcurrent to neutral-current neutrino event rates and their time profiles with respect to each other can provide a handle on supernova and non-standard neutrino physics (mass and flavor oscillations).

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First observation of the neutral current nuclear excitation 12C(v,v′)12C∗(1+, 1)

Cited by 70 publications

References 10 publications

Evidence forν¯μ→ν¯eOscillation

Evidence forν¯μ→ν¯eOscillation

Results onνμ→νeoscillations from pion decay in flight neutrinos

Supernova neutrino detection in Borexino

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