Cerenkov Detector

2016 ◽  
Author(s):  
M. De Bruin
Keyword(s):  
Cerenkov Detector

Optimization of a novel Cerenkov detector for radiotherapy applications using GEANT4 and FLUKA

2011 ◽  
Author(s):  
S. Lo Meo ◽  
T. Rovelli ◽  
C. Fiorino ◽  
G. M. Cattaneo ◽  
R. Calandrino ◽  
...  
Keyword(s):  
Cerenkov Detector

Stability and calibration of a water Čerenkov detector prototype

1999 ◽  
Vol 75 (1-2) ◽  
pp. 389-391
Author(s):  
J.C. D`Olivo ◽  
A. Fernández ◽  
M. Medina ◽  
L. Nellen ◽  
S. Roman ◽  
...  
Keyword(s):  
Cerenkov Detector

Monitoring the energy variation of an electron linac using a Cerenkov detector

2010 ◽  
Vol 34 (1) ◽  
pp. 126-130 ◽  
Author(s):  
Li Shu-Wei ◽  
Wang Yi ◽  
Li Jin ◽  
Li Yuan-Jing ◽  
Kang Ke-Jun ◽  
...  
Keyword(s):  
Electron Linac ◽  
Cerenkov Detector ◽  
Energy Variation

scholarly journals Gas-Čerenkov Detector for 10 to 100 MeV Gamma Rays

1971 ◽  
Vol 41 ◽  
pp. 77-78 ◽  
Author(s):  
H. Helmken ◽  
J. Hoffman
Keyword(s):  
Gamma Radiation ◽  
Point Source ◽  
Gamma Rays ◽  
Angular Resolution ◽  
Galactic Plane ◽  
Plastic Scintillator ◽  
Spectral Information ◽  
Cerenkov Detector ◽  
Half Angle ◽  
Cerenkov Light

A gas-Čerenkov detector sensitive to gamma radiation above 10 MeV is currently undergoing final testing. The detector relies on the conversion and Compton scattering of gamma rays in a plastic scintillator and detecting the resulting electrons via the Čerenkov light they emit in a 2-m propane-gas column. Spectral information can be attained by varying gas pressure during the flight. The present detector is approximately 34″ in diameter, 91″ in length and weight 450 lb. At 20 MeV, an angular resolution of 6° half angle is expected. With an efficiency of 1 to 2%, a 10 hr balloon-borne system should achieve a point-source sensitivity of approximately 5× 10−5 photon cm−2 s−1 above 20 MeV. A satellite version of the detector is expected to have a sensitivity of approximately 1.3 × 10−5 photon cm−2 s−1 above 10 MeV for a 1-month galactic-plane scan mode. (Helmken and Hoffman, 1970.)

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 Resolution Focusing Čerenkov Detector for High Energy Particles

1961 ◽  
Vol 32 (2) ◽  
pp. 111-117 ◽  
Author(s):  
D. A. Hill ◽  
D. O. Caldwell ◽  
D. H. Frisch ◽  
L. S. Osborne ◽  
D. M. Ritson ◽  
...  
Keyword(s):  
High Resolution ◽  
High Energy ◽  
Cerenkov Detector ◽  
High Energy Particles
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