scholarly journals Measurement of the electron neutrino charged-current interaction rate on water with the T2K ND280π0detector

2015 ◽  
Vol 91 (11) ◽  
Author(s):  
K. Abe ◽  
J. Adam ◽  
H. Aihara ◽  
C. Andreopoulos ◽  
S. Aoki ◽  
...  
Keyword(s):  
Electron Neutrino ◽  
Charged Current ◽  
Interaction Rate ◽  
Current Interaction

scholarly journals Charged-Current Interaction Measurements in MiniBooNE

2007 ◽  
Author(s):  
Teppei Katori ◽  
Geralyn P. Zeller ◽  
Jorge G. Morfin ◽  
Flavio Cavanna ◽  
Keyword(s):  
Charged Current ◽  
Current Interaction

NEUTRINO ENERGY LOSS AT MATTER-RADIATION DECOUPLING PHASE

2009 ◽  
Vol 24 (11n13) ◽  
pp. 1051-1054
Author(s):  
UNGKU FERWANI SALWA UNGKU IBRAHIM ◽  
NOR SOFIAH AHMAD ◽  
NORHASLIZA YUSOF ◽  
HASAN ABU KASSIM
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Electron Neutrino ◽  
Stopping Power ◽  
Power Equation ◽  
Electron Positron ◽  
Extra Energy ◽  
Expansion Of The Universe ◽  
Current Interaction ◽  
The Universe

Neutrinos are produced copiously in the early universe. Neutrinos and antineutrinos ceased to be in equilibrium with radiation when the weak interaction rate becomes slower than the rate expansion of the universe. The ratio of the temperature of the photon to the temperature of the neutrino at this stage is Tγ/Tν = (11/4)1/3. We investigate the neutrino energy loss due to the oscillation of the electron neutrino into a different flavor in the charged-current interaction of νe-e- based on the work of Sulaksono and Simanjuntak. The energy loss from the neutrinos ΔEν during the decoupling of the neutrinos with the rest of the matter would be a gain in the energy of the electrons and can be obtained from the integration of stopping power equation ΔEν = (dEν/dT-1)dT-1 where Eν and T are the energy of the neutrinos and the temperature respectively. When the universe expands and matter-radiation decouples, an extra energy will be transferred to the photons via the annihilation of the electron-positron pairs, e++e-→γ+γ. This consequently will increase the temperature of the photons. The net effect to the lowest order is an increase in the ratio of the photon temperature to the neutrino temperature. The magnitude of energy loss of the neutrino is ∼10-4-10-5 MeV for the probability of conversion of νe → νi (i = μ,τ) between 0 to 1.0.

scholarly journals Measurement of the charged-current electron (anti-)neutrino inclusive cross-sections at the T2K off-axis near detector ND280

2020 ◽  
Vol 2020 (10) ◽  
Author(s):  
K. Abe ◽  
◽  
N. Akhlaq ◽  
R. Akutsu ◽  
A. Ali ◽  
...  
Keyword(s):  
Cross Sections ◽  
Electron Neutrino ◽  
Neutrino Beam ◽  
Charged Current ◽  
Total Cross Sections ◽  
Neutrino Scattering ◽  
Near Detector ◽  
Current Electron ◽  
Inclusive Electron ◽  
Selection Of

Abstract The electron (anti-)neutrino component of the T2K neutrino beam constitutes the largest background in the measurement of electron (anti-)neutrino appearance at the far detector. The electron neutrino scattering is measured directly with the T2K off-axis near detector, ND280. The selection of the electron (anti-)neutrino events in the plastic scintillator target from both neutrino and anti-neutrino mode beams is discussed in this paper. The flux integrated single differential charged-current inclusive electron (anti-)neutrino cross-sections, dσ/dp and dσ/d cos(θ), and the total cross-sections in a limited phase-space in momentum and scattering angle (p > 300 MeV/c and θ ≤ 45°) are measured using a binned maximum likelihood fit and compared to the neutrino Monte Carlo generator predictions, resulting in good agreement.

RESULTS FROM THE PURE D2O PHASE OF THE SUDBURY NEUTRINO OBSERVATORY

2003 ◽  
Vol 18 (22) ◽  
pp. 3789-3807
Author(s):  
◽  
F. A. DUNCAN
Keyword(s):  
Neutral Current ◽  
Solar Neutrinos ◽  
Total Flux ◽  
Sudbury Neutrino Observatory ◽  
Charged Current ◽  
Mixing Angle ◽  
Cerenkov Detector ◽  
Neutrino Spectrum ◽  
Oscillation Analysis ◽  
Current Interaction

The Sudbury Neutrino Observatory is a 1000 T D2O Cerenkov detector that is sensitive to 8 B and hep solar neutrinos. Both Charged Current and Neutral Current interaction rates on deuterons as well as the Elastic Scattering interaction rate on electrons can be measured simultaneously. Assuming an undistorted 8 B neutrino spectrum, the total flux measured with the NC reaction is [Formula: see text], which is consistent with solar models. The νe component of the 8 B solar flux is [Formula: see text] for a kinetic energy threshold of 5 MeV. The non-νe component is [Formula: see text], which is 5.3σ greater than zero, giving strong evidence for solar νe flavor transformation. The Day-Night Asymmetry for the Charged Current interaction is [Formula: see text]. If the total flux of active neutrinos is additionally constrained to have no asymmetry, the νe asymmetry is found to be [Formula: see text]. Combined with other solar neutrino data, a global MSW oscillation analysis strongly favors the Large Mixing Angle (LMA) solution.

HIGH-ENERGY NEUTRINO ASTRONOMY WITH THE ANTARES TELESCOPE

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1285-1292
Author(s):  
◽  
P. VERNIN
Keyword(s):  
Three Dimensional ◽  
High Energy ◽  
Charged Current ◽  
Muon Neutrinos ◽  
The Earth ◽  
High Energy Muon ◽  
First Results ◽  
Current Interaction ◽  
Neutrino Astronomy ◽  
Galactic Sources

Since its completion in 2008, ANTARES is the largest neutrino telescope operating in the Northern hemisphere. High-energy muon-neutrinos originating from galactic and extra-galactic sources cross the earth and produce up-going muons by charged current interaction in the medium just below the bottom of the sea or in the water around it. These muons travel through the water with the emission of Cerenkov light detected by a three-dimensional array of photomultipliers tubes (PMT). The performances and the first results of the telescope will be discussed.

Sign in / Sign up

Export Citation Format

Share Document