Electron temperature determination in low-density plasmas from the He I 3889 AA and 5016 AA line intensities

1980 ◽  
Vol 13 (8) ◽  
pp. 1459-1475 ◽  
Author(s):  
N Brenning
Keyword(s):  
Electron Temperature ◽  
Low Density ◽  
Temperature Determination ◽  
Line Intensities

Electron temperature determination in a low density helium plasma

1970 ◽  
Vol 12 (11) ◽  
pp. 897-899 ◽  
Author(s):  
D Schieber ◽  
S Gavril ◽  
M S Erlicki
Keyword(s):  
Electron Temperature ◽  
Helium Plasma ◽  
Low Density ◽  
Temperature Determination

scholarly journals Temperature and Lifetime Measurements in the SSX Wind Tunnel

Plasma ◽  
2018 ◽  
Vol 1 (2) ◽  
pp. 229-241 ◽  
Author(s):  
Manjit Kaur ◽  
Kaitlin Gelber ◽  
Adam Light ◽  
Michael Brown
Keyword(s):  
Simple Model ◽  
Wind Tunnel ◽  
Electron Temperature ◽  
Langmuir Probe ◽  
Vacuum Ultraviolet ◽  
Lifetime Measurements ◽  
Line Intensities ◽  
Thermal Equilibration ◽  
Local Measurements ◽  
Doppler Spectroscopy

We describe ion and electron temperature measurements in the Swarthmore Spheromak Experiment (SSX) MHD wind tunnel with the goal of understanding limitations on the lifetime of our Taylor-state plasma. A simple model based on the equilibrium eigenvalue and Spitzer resistivity predicted the lifetime satisfactorily during the first phase of the plasma evolution. We measured an average T e along a chord by taking the ratio of the C I I I 97.7 nm to C I V 155 nm line intensities using a vacuum ultraviolet (VUV) monochromator. We also recorded local measurements of T e and n e using a double Langmuir probe in order to inform our interpretation of the VUV data. Our results indicated that the plasma decayed inductively during a large part of the evolution. Ion Doppler spectroscopy measurements suggested that ions cooled more slowly than would be expected from thermal equilibration with the electrons, which maintained a constant temperature throughout the lifetime of the plasma.

scholarly journals Spotty appearance of the solar disk as inferred from the comparaison between EUV and radio intensities

1965 ◽  
Vol 23 ◽  
pp. 109-114
Author(s):  
Z. Suemoto ◽  
F. Moriyama
Keyword(s):  
Electron Temperature ◽  
Transition Layer ◽  
Solar Disk ◽  
Sunspot Minimum ◽  
Line Intensities ◽  
Inhomogeneous Model ◽  
First Approximation

This is a revised version of the work reported to the COSPAR Symposium of 1962. In the first place, the basic components of the radio intensities ranging from 1000 MHz to 9400 MHz derived by H. Tanaka were used to establish the relation between the electron temperature and integrated number of electrons for 1960 and 1961 flights. The result justifies our former assumption that the radio intensities with which the EUV line intensities from the transition layer are to be compared should, as a first approximation, be very close to those at sunspot minimum.In the second place, the integrated numbers of electrons from the EUV line intensities were derived based on the same data as were used by Pottasch. This is to eliminate any arbitrariness in adopting parameters which are still uncertain.The result is that we still have a large amount of disagreement between the two sets of intensities in the sense that EUV line intensities are at least ten times stronger as might be inferred from the radio intensities. If one assumes an inhomogeneous model in which the solar disk is bright only in patches covering about 0.15 of its total area, the discrepancy would be eliminated.

Temporal and Spatial Behavior of Electron Density and Temperature in a Laser-Produced Plasma from YBa2Cu3O7

1998 ◽  
Vol 52 (3) ◽  
pp. 449-455 ◽  
Author(s):  
S. S. Harilal ◽  
C. V. Bindhu ◽  
V. P. N. Nampoori ◽  
C. P. G. Vallabhan
Keyword(s):  
Electron Temperature ◽  
Electron Density ◽  
Spectroscopic Studies ◽  
Spatial Behavior ◽  
Laser Irradiance ◽  
Stark Broadening ◽  
Line Intensities ◽  
Experimental Parameters ◽  
Temporal And Spatial

Spectroscopic studies of laser-induced plasma from a high-temperature superconducting material, viz., YBa2Cu3O7 (YBCO), have been carried out. Electron temperature and electron density measurements were made from spectral data. The Stark broadening of emission lines was used to determine the electron density, and the ratio of line intensities was exploited for the determination of electron temperature. An initial electron temperature of 2.35 eV and electron density of 2.5 × 1017 cm−3 were observed. The dependence on electron temperature and density on different experimental parameters such as distance from the target, delay time after the initiation of the plasma, and laser irradiance is also discussed in detail.

scholarly journals The Cu I And Zn I-Like Spectra of Pr, Eu, Gd, Dy And Yb Emitted by a Tokamak Plasma in the 50–200 Å Range

1988 ◽  
Vol 102 ◽  
pp. 75-77
Author(s):  
W.L. Hodge ◽  
M. Finkenthal ◽  
H.W. Moos ◽  
S. Lippmann ◽  
L.K. Huang ◽  
...  
Keyword(s):  
Rare Earth ◽  
High Temperature ◽  
Grazing Incidence ◽  
Spectral Lines ◽  
Tokamak Plasma ◽  
Low Density ◽  
Line Intensities ◽  
Time Histories ◽  
Collisional Radiative Model ◽  
Radiative Model

AbstractSpectra of rare earth elements, praseodymium, europium, gadolinium, dysprosium and ytterbium (Z=59 to Z=70) have been recorded from a high temperature (Te=1–1.4 keV) - low density (ne=1013cm−3) tokamak plasma, in the 50–200 Å range. The absolute brightnesses of the lines originating in 4–4 transitions of Cu I and Zn I-like ions of the above mentioned elements have been measured by means of a photometrically calibrated grazing incidence spectrometer. Newly identified Cu I-like, 4s2S1/2-4p2P1/2transitions in Pr30+, Eu34+, Gd35+, Dy37+and Yb41, and intercombination transitions 4s21S0-4s4p3P1, in the Zn I-like ions of the mentioned elements are presented. The identifications are based on interpolation of previous experimental results, ab initio energy level computations using the RELAC code and are substantiated by the time histories of individual spectral lines. The experimental line intensities of the Cu I and Zn I-like ions are compared with those predicted by a collisional-radiative model under the conditions of the tokamak plasma.

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