Dynamical thermoelectric coefficients of bulk semiconductor crystals: Towards high thermoelectric efficiency at high frequencies

2014 ◽  
Vol 115 (22) ◽  
pp. 223703 ◽  
Author(s):  
Younès Ezzahri ◽  
Karl Joulain
Keyword(s):  
Thermoelectric Efficiency ◽  
High Frequencies ◽  
Semiconductor Crystals ◽  
Bulk Semiconductor

Persistent light-induced change in the effective band gap and reversible control over the effective band gap in bulk semiconductor crystals

2011 ◽  
Vol 83 (24) ◽  
Author(s):  
Sharon Shwartz ◽  
K. V. Adarsh ◽  
Mordechai Segev ◽  
Evgeny Lakin ◽  
Emil Zolotoyabko ◽  
...  
Keyword(s):  
Band Gap ◽  
Semiconductor Crystals ◽  
Bulk Semiconductor

On the high growth rates in electroepitaxial growth of bulk semiconductor crystals in magnetic field

2005 ◽  
Vol 275 (1-2) ◽  
pp. e1-e6 ◽  
Author(s):  
Sadik Dost ◽  
Hamdi Sheibani ◽  
Yongcai Liu ◽  
Brian Lent
Keyword(s):  
Magnetic Field ◽  
Growth Rates ◽  
High Growth ◽  
Semiconductor Crystals ◽  
Bulk Semiconductor

Dynamical thermal conductivity of bulk semiconductor crystals

2012 ◽  
Vol 112 (8) ◽  
pp. 083515 ◽  
Author(s):  
Younès Ezzahri ◽  
Karl Joulain
Keyword(s):  
Thermal Conductivity ◽  
Semiconductor Crystals ◽  
Bulk Semiconductor

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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