FARADAIC RECTIFICATION AND ELECTRODE PROCESSES. III. EXPERIMENTAL METHODS FOR HIGH FREQUENCIES AND APPLICATION TO THE DISCHARGE OF MERCUROUS ION

1962 ◽  
Vol 66 (6) ◽  
pp. 1108-1113 ◽  
Author(s):  
Hideo Imai ◽  
Paul Delahay
Keyword(s):  
Experimental Methods ◽  
High Frequencies ◽  
Electrode Processes ◽  
Mercurous Ion ◽  
Faradaic Rectification

FARADAIC RECTIFICATION AND ELECTRODE PROCESSES. II

1961 ◽  
Vol 65 (7) ◽  
pp. 1253-1256 ◽  
Author(s):  
Mitsugi Senda ◽  
Hideo Imai ◽  
Paul Delahay
Keyword(s):  
Electrode Processes ◽  
Faradaic Rectification

Use of Faradaic Rectification for the Study of Rapid Electrode Processes

Nature ◽  
1958 ◽  
Vol 181 (4604) ◽  
pp. 247-248 ◽  
Author(s):  
G. C. BARKER ◽  
R. L. FAIRCLOTH ◽  
A. W. GARDNER
Keyword(s):  
Electrode Processes ◽  
Faradaic Rectification

scholarly journals Faradaic Rectification and Electrode Processes

1961 ◽  
Vol 83 (2) ◽  
pp. 312-322 ◽  
Author(s):  
Paul Delahay ◽  
Mitsugi Senda ◽  
Carl H. Weis
Keyword(s):  
Electrode Processes ◽  
Faradaic Rectification

Quasi-Periodic Oscillations in Dwarf Novae

1979 ◽  
Vol 46 ◽  
pp. 77-88
Author(s):  
Edward L. Robinson
Keyword(s):  
Binary Systems ◽  
Outer Edge ◽  
Light Curves ◽  
Close Binary ◽  
Bright Spot ◽  
Dwarf Novae ◽  
Periodic Oscillations ◽  
High Frequencies ◽  
Short Period ◽  
Typical Time

Three distinct kinds of rapid variations have been detected in the light curves of dwarf novae: rapid flickering, short period coherent oscillations, and quasi-periodic oscillations. The rapid flickering is seen in the light curves of most, if not all, dwarf novae, and is especially apparent during minimum light between eruptions. The flickering has a typical time scale of a few minutes or less and a typical amplitude of about .1 mag. The flickering is completely random and unpredictable; the power spectrum of flickering shows only a slow decrease from low to high frequencies. The observations of U Gem by Warner and Nather (1971) showed conclusively that most of the flickering is produced by variations in the luminosity of the bright spot near the outer edge of the accretion disk around the white dwarf in these close binary systems.

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