Plasma line broadening and computer simulations: A mini-review

Stambulchik, E.; Maron, Y.

doi:10.1016/j.hedp.2009.07.001

Cited by 48 publications

(38 citation statements)

References 47 publications

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“…The profiles obtained considering specific experimental conditions allow researchers to undertake plasma diagnostics by direct comparison of the line profiles obtained in the simulations and those experimentally recorded. More details on CSM for line shapes calculations can be found in the review [83].…”

Section: I(ωe) Is the Broadened Profile Due To The Impact Electrons mentioning

confidence: 99%

Electron density measurement in atmospheric pressure plasma jets: Stark broadening of hydrogenated and non-hydrogenated lines

Nikiforov

Leys

González

et al. 2015

Plasma Sources Sci. Technol.

205

179

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Electron density is one of the key parameters in the physics of a gas discharge. In this contribution the application of the Stark broadening method to determine the electron density in low temperature atmospheric pressure plasma jets is discussed. An overview of the available theoretical Stark broadening calculations of hydrogenated and non-hydrogenated atomic lines is presented. The difficulty in the evaluation of the fine structure splitting of lines, which is important at low electron density, is analysed and recommendations on the applicability of the method for low ionization degree plasmas are given. Different emission line broadening mechanisms under atmospheric pressure conditions are discussed and an experimental line profile fitting procedure for the determination of the Stark broadening contribution is suggested. Available experimental data is carefully analysed for the Stark broadening of lines in plasma jets excited over a wide range of frequencies from dc to MW and pulsed mode. Finally, recommendations are given concerning the application of the Stark broadening technique for the estimation of the electron density under typical conditions of plasma jets.

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Section: I(ωe) Is the Broadened Profile Due To The Impact Electrons mentioning

confidence: 99%

Electron density measurement in atmospheric pressure plasma jets: Stark broadening of hydrogenated and non-hydrogenated lines

Nikiforov

Leys

González

et al. 2015

Plasma Sources Sci. Technol.

205

179

View full text Add to dashboard Cite

show abstract

“…This exception becomes less important for the higher members of the Balmer series. Besides numerical simulations [7] an analytical unified description of the electrons and ions can be done with the model microfield method (MMM), derived by Brissaud and Frisch [8]. Here, time dependent electric micro fields produced by the plasma electrons and ions are introduced, where the field strength jumps instantaneously between constant values in a stochastic way [9,10].…”

Section: Theory Of Stark Broadening In a Plasmamentioning

confidence: 99%

Electron density determination in the divertor volume of ASDEX Upgrade via Stark broadening of the Balmer lines

Potzel

Dux

Müller

et al. 2014

Plasma Phys. Control. Fusion

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Abstract. In this article we present the development of a new diagnostic capable of determining the electron density in the divertor volume of ASDEX Upgrade. It is based on the spectroscopic measurement of the Stark broadening of the Balmer lines. In this work two approaches of calculating the Stark broadening, i.e. the unified theory and the model microfield method, are compared. It will be shown that both approaches yield similar results in the case of Balmer lines with high upper principal quantum numbers n. In addition, for typical ASDEX Upgrade parameters the influence of the Zeeman splitting on the high n Balmer lines is found to be negligible. Moreover, an assumption for the Doppler broadening of T n = 5 eV, which is the maximum FrankCondon dissociation energy of recycled neutrals, is sufficient. The initial electron density measurements performed using this method are found to be consistent with both Langmuir probe and pressure gauge data.

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“…The ion dynamics leads to an additional broadening, which can be important especially at low densities, high temperatures, or for lines with a low upper principal quantum number. Simulations involving a numerical integration of the Liouville Equation (3) and not referring to Equation (5) can also be performed, but they become time-consuming if the atomic system is complex [7,14,15].…”

Section: Stark Line Shape Modelingmentioning

confidence: 99%

A New Analysis of Stark and Zeeman Effects on Hydrogen Lines in Magnetized DA White Dwarfs

Kieu

Rosato

Stamm

et al. 2017

Atoms

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White dwarfs with magnetic field strengths larger than 10 T are understood to represent more than 10% of the total population of white dwarfs. The presence of such strong magnetic fields is clearly indicated by the Zeeman triplet structure visible on absorption lines. In this work, we discuss the line broadening mechanisms and focus on the sensitivity of hydrogen lines on the magnetic field. We perform new calculations in conditions relevant to magnetized DA stellar atmospheres using models inspired from magnetic fusion plasma spectroscopy. A white dwarf spectrum from the Sloan Digital Sky Survey (SDSS) database is analyzed. An effective temperature is provided by an adjustment of the background radiation with a Planck function, and the magnetic field is inferred from absorption lines presenting a Zeeman triplet structure. An order-of-magnitude estimate for the electron density is also performed from Stark broadening analysis.

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Plasma line broadening and computer simulations: A mini-review

Cited by 48 publications

References 47 publications

Electron density measurement in atmospheric pressure plasma jets: Stark broadening of hydrogenated and non-hydrogenated lines

Electron density measurement in atmospheric pressure plasma jets: Stark broadening of hydrogenated and non-hydrogenated lines

Electron density determination in the divertor volume of ASDEX Upgrade via Stark broadening of the Balmer lines

A New Analysis of Stark and Zeeman Effects on Hydrogen Lines in Magnetized DA White Dwarfs

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