Determination of Electron Temperature from Emission Intensity Ratios in Line Spectra

1971 ◽  
pp. 39-67
Author(s):  
I. M. Podgornyi
Keyword(s):  
Electron Temperature ◽  
Emission Intensity ◽  
Intensity Ratios

Saha-Boltzmann Statistics for Determination of Electron Temperature and Density in Spark Discharges Using an Echelle/CCD System

1993 ◽  
Vol 47 (12) ◽  
pp. 2022-2030 ◽  
Author(s):  
Cheryl A. Bye ◽  
Alexander Scheeline
Keyword(s):  
Electron Temperature ◽  
Spectral Information ◽  
Sample Matrix ◽  
Spark Discharges ◽  
Multiple Ionization ◽  
Nonequilibrium Conditions ◽  
Intensity Ratios ◽  
Spectrometer System ◽  
Nonequilibrium Excitation

A custom echelle/CCD spectrometer system has been employed for equilibrium and nonequilibrium excitation measurements in the high-voltage spark discharge. By exploitation of the large spectral information bandwidth of the echelle/CCD system, multiple ionization stages of argon were observed in the spark emission spectrum. Ion-to-atom emission intensity ratios were used in a linearized form of the coupled Saha-Boltzmann equation for the determination of both electron temperature and density. Nonequilibrium conditions were considered. The dependence of argon excitation on sample matrix was also explored.

scholarly journals A physico-chemical model to study the ion density distribution in the inner coma of comet C/2016 R2 (Pan-STARRS)

2020 ◽  
Author(s):  
Susarla Raghuram ◽  
Anil Bhardwaj ◽  
Damien Hutsemékers ◽  
Cyrielle Opitom ◽  
Jean Manfroid ◽  
...  
Keyword(s):  
Density Distribution ◽  
Electron Impact ◽  
Emission Intensity ◽  
Impact Ionization ◽  
Excitation Source ◽  
Resonance Fluorescence ◽  
Ion Density ◽  
Physico Chemical ◽  
Intensity Ratios ◽  
Ion Emission

Abstract The recent observations show that comet C/2016 R2 (Pan-Starrs) has a unique and peculiar composition when compared with several other comets observed at 2.8 au heliocentric distance. Assuming solar resonance fluorescence is the only excitation source, the observed ionic emission intensity ratios are used to constrain the corresponding neutral abundances in this comet. We developed a physico-chemical model to study the ion density distribution in the inner coma of this comet by accounting for photon and electron impact ionization of neutrals, charge exchange and proton transfer reactions between ions and neutrals, and electron-ion thermal recombination reactions. Our calculations show that CO$_2^+$ and CO+ are the major ions in the inner coma, and close to the surface of nucleus CH3OH+, CH3OH$_2^+$ and O$_2^+$ are also important ions. By considering various excitation sources, we also studied the emission mechanisms of different excited states of CO+, CO$_2^+$, N$_2^+$, and H2O+. We found that the photon and electron impact ionization and excitation of corresponding neutrals significantly contribute to the observed ionic emissions for radial distances smaller than 300 km and at larger distances, solar resonance fluorescence is the major excitation source. Our modelled ion emission intensity ratios are consistent with the ground-based observations. Based on the modelled emission processes, we suggest that the observed ion emission intensity ratios can be used to derive the neutral composition in the cometary coma only when the ion densities are significantly controlled by photon and photoelectron impact ionization of neutrals rather than by the ion-neutral chemistry.

scholarly journals The Stark-crossing method for the simultaneous determination of the electron temperature and density in plasmas

2006 ◽  
Vol 44 ◽  
pp. 70-79 ◽  
Author(s):  
J Torres ◽  
O Carabaño ◽  
M Fernández ◽  
S Rubio ◽  
R Álvarez ◽  
...  
Keyword(s):  
Electron Temperature ◽  
Simultaneous Determination

scholarly journals The broad line region of AGN: Kinematics and physics

2006 ◽  
pp. 1-11 ◽  
Author(s):  
L.C. Popovic
Keyword(s):  
Electron Temperature ◽  
Accretion Disk ◽  
Emission Lines ◽  
Physical Parameters ◽  
Broad Line ◽  
Physical Conditions ◽  
Broad Line Region ◽  
Broad Emission ◽  
Line Region

In this paper a discussion of kinematics and physics of the Broad Line Region (BLR) is given. The possible physical conditions in the BLR and problems in determination of the physical parameters (electron temperature and density) are considered. Moreover, one analyses the geometry of the BLR and the probability that (at least) a fraction of the radiation in the Broad Emission Lines (BELs) originates from a relativistic accretion disk.

Measurement Of Relative X-Ray Intensity Ratios for Elements With Z=14 to 92 Using EDXRF Spectrometer

1993 ◽  
Vol 37 ◽  
pp. 697-709 ◽  
Author(s):  
Krassimir N. Stoev ◽  
Joseph F. Dlouhy
Keyword(s):  
Fluorescence Analysis ◽  
Radiative Transition ◽  
Published Data ◽  
Emission Rates ◽  
Experimental Physics ◽  
X Ray ◽  
Overlapped Peaks ◽  
Intensity Ratios ◽  
Atomic Structure Calculations

Nowadays x-ray fluorescence analysis is one of the major techniques for determination of trace elements. Vacuum operated Si (Li) .energy-dispersive x-ray spectrometers can analyze simultaneously up to 50 elements from Na (Z=11) to U (Z = 92) . Proper interpretation of the accumulated spectra requires correct solution of x-ray line overlap problems. In many cases knowledge of x-ray intensity ratios can make the procedure for resolving the overlapped peaks more reliable and reproducible. Measurements of radiative transition rates can also provide fundamental tests of theoretical atomic structure calculations. There are many other useful applications of x-ray emission rates in theoretical and experimental physics. On the other hand, there are differences in the published data, which suggests that x-ray intensity ratios are still not known with the necessary accuracy, and new measurements are useful and necessary.

scholarly journals Diffuse Interstellar Bands – The Unidentified Part of the Interstellar Absorption Spectrum

1989 ◽  
Vol 135 ◽  
pp. 67-86 ◽  
Author(s):  
Jacek Krełowski
Keyword(s):  
Absorption Spectrum ◽  
Line Of Sight ◽  
Optical Parameters ◽  
Interstellar Matter ◽  
Molecular Absorption ◽  
Interstellar Clouds ◽  
Diffuse Interstellar Bands ◽  
Intensity Ratios ◽  
Molecular Abundances

The unidentified (since 1921) diffuse interstellar bands (DIBs) are discussed together with their relations to other interstellar absorptions sucn as: continuous extinction, polarization and atomic or molecular absorption lines. It is shown that DIBs do not form the absorption spectrum of one agent, but probably of several (3 or more). DIBs as well as other interstellar absorptions are usually formed in several clouds along a line-of-sight. Thus, they suffer Doppler splitting; the first high resolution profiles free of the latter effect are described. Since single interstellar clouds may differ not only in radial velocities but also in many physical (optical) parameters, the observed interstellar absorptions are ill-defined averages over all clouds situated along any line-of-sight. It is of basic importance to determine not only the single cloud profiles of diffuse bands, but also their relations to other interstellar absorptions in the same clouds. Intensity ratios of DIBs are shown to be sensitive to the shapes of extinction curves, depletion patterns of elements and molecular abundances in the considered clouds. The sensitivity of the DIBs to the variation in polarization is less documented but probably also present. Thus the diffuse lines are presented as the unidentified part of the absorption spectrum of interstellar matter. Their identification depends on the determination of their relations to other interstellar absorptions which must be determined precisely.

scholarly journals Microalbuminuria and borderline-increased albumin excretion determined with a centrifugal analyzer and the Albumin Blue 580 fluorescence assay

1997 ◽  
Vol 43 (6) ◽  
pp. 996-1002 ◽  
Author(s):  
Manfred A Kessler ◽  
Andreas Meinitzer ◽  
Walter Petek ◽  
Otto S Wolfbeis
Keyword(s):  
Calibration Curve ◽  
Emission Intensity ◽  
Clinical Laboratory ◽  
Detection Limits ◽  
High Specificity ◽  
Fluorescence Assay ◽  
Urine Samples ◽  
Albumin Concentration ◽  
Specificity And Sensitivity

Abstract We report a new automated fluorescence assay for determination of albumin in urine. The dye Albumin Blue 580 specifically binds to albumin with exhibition of strong red fluorescence. The albumin concentration is calculated from emission intensity at 616 nm (excitation at 590 nm) and a calibration curve. Two Cobas Fara programs cover working ranges of 2–200 and 1–50 mg/L with detection limits of 1.4 and 0.4 mg/L, respectively. Within-run CVs (n = 10) ranged from 1.7% (189 mg/L) to 8.9% (7.2 mg/L) for 2–200 mg/L and from 2.9% (43.3 mg/L) to 5.7% (2.3 mg/L) for the 1–50 mg/L range. A test of urine samples (n = 100) submitted to routine analysis gave results that agreed well with those by the Behring nephelometric assay: AB 580 = 0.922 (± 0.010) BNA + 4.16 (± 0.78). No interference was detected from other urine components, including several proteins and 46 drugs. The high specificity and sensitivity make the method ideal for determination of microalbuminuria. In addition, the method is fast, inexpensive, and well-suited for clinical laboratory application and thus may be used instead of immunoassays.

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