Study on the stability of 20 inch photomultiplier tubes based on microchannel plate

2021 ◽  
Vol 16 (06) ◽  
pp. T06015
Author(s):  
H. Li ◽  
S. Qian ◽  
Z. Ning ◽  
Y. Zhang ◽  
Q. Wu ◽  
...  
Keyword(s):  
Microchannel Plate ◽  
Photomultiplier Tubes ◽  
The Stability

Analogue saturation limit of single and double 10 mm microchannel plate photomultiplier tubes

2016 ◽  
Vol 87 (11) ◽  
pp. 11D832 ◽  
Author(s):  
J. S. Milnes ◽  
T. M. Conneely ◽  
C. J. Horsfield
Keyword(s):  
Microchannel Plate ◽  
Photomultiplier Tubes ◽  
Saturation Limit

scholarly journals Area and extraction field analysis of the analogue saturation of 40 mm microchannel plate photomultiplier tubes

2018 ◽  
Vol 89 (10) ◽  
pp. 10K104 ◽  
Author(s):  
J. S. Milnes ◽  
T. M. Conneely ◽  
C. J. Horsfield ◽  
J. Lapington
Keyword(s):  
Microchannel Plate ◽  
Field Analysis ◽  
Photomultiplier Tubes ◽  
Extraction Field

Improved time response for large area microchannel plate photomultiplier tubes in fusion diagnostics

2014 ◽  
Vol 85 (11) ◽  
pp. 11E601 ◽  
Author(s):  
J. S. Milnes ◽  
C. J. Horsfield ◽  
T. M. Conneely ◽  
J. Howorth
Keyword(s):  
Microchannel Plate ◽  
Time Response ◽  
Large Area ◽  
Photomultiplier Tubes ◽  
Fusion Diagnostics

The stability of CsI-coated microchannel plate X-ray detectors

1984 ◽  
Vol 224 (1-2) ◽  
pp. 287-297 ◽  
Author(s):  
M.J. Whiteley ◽  
J.F. Pearson ◽  
G.W. Fraser ◽  
M.A. Barstow
Keyword(s):  
Microchannel Plate ◽  
X Ray ◽  
The Stability

Proximity Focused Microchannel Plate Photomultiplier Tubes

1981 ◽  
Vol 28 (1) ◽  
pp. 677-682 ◽  
Author(s):  
D. H. Ceckowski ◽  
E. Eberhardt ◽  
E. Carney
Keyword(s):  
Microchannel Plate ◽  
Photomultiplier Tubes

Open discussion

1982 ◽  
Vol 99 ◽  
pp. 605-613
Author(s):  
P. S. Conti
Keyword(s):  
Buenos Aires ◽  
Large Mass ◽  
List Type ◽  
Common Phenomenon ◽  
Open Discussion ◽  
The Stability ◽  
Ring Nebulae

Conti: One of the main conclusions of the Wolf-Rayet symposium in Buenos Aires was that Wolf-Rayet stars are evolutionary products of massive objects. Some questions:–Do hot helium-rich stars, that are not Wolf-Rayet stars, exist?–What about the stability of helium rich stars of large mass? We know a helium rich star of ∼40 MO. Has the stability something to do with the wind?–Ring nebulae and bubbles : this seems to be a much more common phenomenon than we thought of some years age.–What is the origin of the subtypes? This is important to find a possible matching of scenarios to subtypes.

Symmetric Multistep Methods Revisited: II. Numerical Experiments

1999 ◽  
Vol 173 ◽  
pp. 309-314 ◽  
Author(s):  
T. Fukushima
Keyword(s):  
Multistep Methods ◽  
Computational Time ◽  
Integration Time ◽  
Implicit Methods ◽  
Symmetric Methods ◽  
Celestial Bodies ◽  
The Stability ◽  
Predictor Corrector ◽  
Symmetric Multistep Methods ◽  
Integration Errors

AbstractBy using the stability condition and general formulas developed by Fukushima (1998 = Paper I) we discovered that, just as in the case of the explicit symmetric multistep methods (Quinlan and Tremaine, 1990), when integrating orbital motions of celestial bodies, the implicit symmetric multistep methods used in the predictor-corrector manner lead to integration errors in position which grow linearly with the integration time if the stepsizes adopted are sufficiently small and if the number of corrections is sufficiently large, say two or three. We confirmed also that the symmetric methods (explicit or implicit) would produce the stepsize-dependent instabilities/resonances, which was discovered by A. Toomre in 1991 and confirmed by G.D. Quinlan for some high order explicit methods. Although the implicit methods require twice or more computational time for the same stepsize than the explicit symmetric ones do, they seem to be preferable since they reduce these undesirable features significantly.

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