Optimization of Beat Frequency Plasma Heating near the Electron Cyclotron Frequency

1974 ◽  
Vol 52 (22) ◽  
pp. 2223-2227 ◽  
Author(s):  
C. E. Capjack ◽  
C. R. James
Keyword(s):  
Cyclotron Frequency ◽  
Plasma Heating ◽  
Beat Frequency ◽  
Laser Beams ◽  
Plasma Power ◽  
Electron Current ◽  
Frequency Wave ◽  
Parametric Dependence ◽  
Frequency Plasma ◽  
Nonlinear Mixing

The plasma power absorbed from a beat frequency wave generated through the nonlinear mixing of two laser beams may be optimized by the utilization of an electron current resonance. The parametric dependence of the plasma power absorption near an electron resonance is examined together with experimental considerations for the case where CO2 lasers are used.

Liquid nitrogen cooled window for high frequency plasma heating

1994 ◽  
Vol 212-215 ◽  
pp. 1035-1038 ◽  
Author(s):  
H.E. Häfner ◽  
E. Bojarsky ◽  
K. Heckert ◽  
P. Norajitra ◽  
H. Reiser
Keyword(s):  
Liquid Nitrogen ◽  
High Frequency ◽  
Plasma Heating ◽  
High Frequency Plasma ◽  
Frequency Plasma

Transport model of plasma heating at the second harmonic of the electron-cyclotron frequency

2021 ◽  
Author(s):  
Yurii N Dnestrovskij ◽  
Alexander V Danilov ◽  
Alexey Dnestrovskiy ◽  
Sergey E. Lysenko ◽  
Alexander V Melnikov ◽  
...  
Keyword(s):  
Cyclotron Frequency ◽  
Transport Model ◽  
Second Harmonic ◽  
Plasma Heating ◽  
Electron Cyclotron ◽  
Electron Cyclotron Frequency

The Effect of Plasma Power on the Properties of Amorphous Silicon-Germanium Thin Films

2011 ◽  
Vol 317-319 ◽  
pp. 341-344
Author(s):  
Long Gu ◽  
Hui Dong Yang ◽  
Bo Huang
Keyword(s):  
Thin Films ◽  
Amorphous Silicon ◽  
Deposition Rate ◽  
Silicon Germanium ◽  
Structural Characteristics ◽  
Chemical Vapor ◽  
Plasma Power ◽  
Glass Substrates ◽  
Frequency Plasma ◽  
Amorphous Silicon Germanium

Amorphous Silicon-germanium films were prepared by radio frequency plasma enhanced chemical vapor deposition (RF-PECVD) on glass substrates. The structural characteristics, deposition rate, photosensitivity, and optical band gap of the silicon-germanium thin films were investigated with plasma power varying from 15W to 45W. The deposition rate increased within a certain range of plasma power. With the plasma power increasing, the photosensitivity of the thin films decreased. It is evident that varying the plasma power changes the deposition rate, photosensitivity, which was fundamentally crucial for the fabrication of a-Si/a-SiGe/a-SiGe stacked solar cells. For our deposition system, the most optimization value was 30-35W.

Feasibility of rf plasma heating in the Globus-M spherical tokamak at frequencies above the ion cyclotron frequency

2003 ◽  
Vol 48 (8) ◽  
pp. 1061-1066
Author(s):  
V. V. D’yachenko ◽  
M. A. Irzak ◽  
E. N. Tregubova ◽  
O. N. Shcherbinin
Keyword(s):  
Cyclotron Frequency ◽  
Plasma Heating ◽  
Rf Plasma ◽  
Spherical Tokamak ◽  
Ion Cyclotron

scholarly journals Solar Orbiter’s first Venus Flyby: MAG observations of structures and waves associated with the induced Venusian magnetosphere

2021 ◽  
Author(s):  
Martin Volwerk ◽  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
High Frequency ◽  
Cyclotron Frequency ◽  
Plasma Waves ◽  
Bow Shock ◽  
High Frequency Plasma ◽  
Frequency Plasma ◽  
Mirror Mode ◽  
Proton Cyclotron

<p>The induced magnetosphere of Venus is created by the interaction of the solar wind and embedded interplanetary magnetic field with the exosphere and ionosphere of Venus. Solar Orbiter entered Venus’s magnetotail far downstream, > 70 Venus radii, of the planet and exited the magnetosphere over the north pole. This offered a unique view of the system over distances that were only flown through once by three other missions before, Mariner 10, Galileo and Bepi-Colombo. The large-scale structure and activity of the induced magnetosphere is studied as well as the high-frequency plasma waves both in the magnetosphere and in a limited region upstream of the planet where interaction with Venus’s exosphere is expected.  It is shown that Venus’s magnetotail is very active during the Solar Orbiter flyby. Structures such as flux ropes, and reconnection sites are encountered as well as a strongly overdraping of the magnetic field downstream of the bow shock and planet. High-frequency plasma waves (up to 6 times the local proton cyclotron frequency) are observed in the magnetotail, which are identified as Doppler-shifted proton cyclotron waves, whereas in the upstream solar wind these waves appear just below the proton cyclotron frequency (as expected) but are very patchy. The bow shock is quasi perpendicular, however, expected mirror mode activity is not found directly behind it; instead there is strong cyclotron wave power. This is most-likely caused by the relatively low plasma-beta  behind the bow shock. Much further downstream in the magnetosheath mirror mode of magnetic hole structures are identified. This presentation will take place after the second Venus flyby by Solar Orbiter and BepiColombo and Solar Orbiter on 9 and 10 August, respectively.</p>

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