Stark effect of high-<i>n</i>hydrogen-like transitions: quasi-contiguous approximation

Stambulchik, E.; Maron, Y.

doi:10.1088/0953-4075/41/9/095703

Cited by 50 publications

(62 citation statements)

References 25 publications

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“…(3.51), not present in the original study [10], was empirically found to serve as a rough correction for the ∆n = 1 case; we remind the reader that the QC approximation was derived assuming ∆n ≫ 1). Static/dynamic Stark ratio:…”

Section: Spectroscopymentioning

confidence: 95%

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Plasma formulary interactive

Stambulchik

Maron

2011

J. Inst.

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We present an interactive, Web-based application that provides a comfortable access to evaluating, comparing, and plotting of a multitude of different plasma and atomic physics parameters, grouped by the unit dimensions. A special attention is devoted to the Stark broadening which is calculated with a good accuracy for transitions between degenerate atomic levels. The list of the entities calculated encompasses over one hundred entries and is easily expandable. The application is built using open-source components and is compatible with a majority of modern browsers.

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Section: Spectroscopymentioning

confidence: 95%

“…Typical Debye screening (plasma screening of a Coulomb field exerted by a probe charge at the distance of the Wigner-Seitz radius): The Stark broadening is calculated in the quasi-contiguous (QC) approximation [10], applicable to transitions between degenerate atomic levels. The method is summarized below.…”

Section: Spectroscopymentioning

confidence: 99%

Plasma formulary interactive

Stambulchik

Maron

2011

J. Inst.

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“…Stambulchik and Maron [27] made some advances into approximate analytical calculations of the Stark widths of highly-excited hydrogen/deuterium lines. (They started within the CT, where the ion-dynamical effects are neglected, but then tried to take into account the ion dynamics in a rough approximation).…”

Section: /2 Ementioning

confidence: 99%

Electron Density

2017

Diagnostics of Laboratory and Astrophysical Plasmas Using Spectral Lineshapes of One-, Two-, and Three-Electron Systems

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The electron density N e is the primary plasma parameter. In laboratory and astrophysical plasmas, it varies over 20 orders of magnitude (in distinction to any other plasma parameter): from N e ∼ (10 3 -10 4 ) cm −3 in astrophysical objects called H II regions to N e ∼ (10 23 -10 24 ) cm −3 in plasmas produced by very powerful lasers. (For comparison, the electron temperature T e of these two extreme types of plasmas varies only by about three orders of magnitude: from ∼1 eV in H II regions to ∼1 keV in plasmas produced by very powerful lasers.) Obviously, there is no single universal method for measuring N e that can be applied over 20 orders of magnitude. The overwhelming majority of method for measuring N e are based on Stark broadening (SB) of various spectral lines by ion and electron microfields in plasmas.SB of spectral lines in plasmas is controlled by the electron density N e and to some extent by the electron (T e ) and ion (T i ) temperatures. Therefore, it was used for measuring the electron density in a very broad range by choosing appropriate spectral lines. The experimental determination of the electron density relies mostly on measuring the Stark width because it is typically by an order of magnitude greater than the Stark shift.Hydrogenic radiators are the most appropriate for this purpose. The overwhelming majority of the states of hydrogenic radiators 3 Diagnostics of Laboratory and Astrophysical Plasmas Using Spectral Lineshapes of One-, Two-, and Three-Electron Systems Downloaded from www.worldscientific.com by 34.215.51.103 on 05/10/18. For personal use only. Diagnostics of Laboratory and Astrophysical Plasmaspossess permanent dipole moments, thus, making these radiators more sensitive to ion and electron microfields in plasmas than non-hydrogenic radiators. The underlying theories are presented in Appendices A-E, G-I, and L. In practice, there could be competing broadening mechanisms, such as, Doppler, instrumental and Zeeman broadenings, as well as a self-absorption. Therefore, the task is to find practical methods for extracting the Stark width despite the competing broadening effects, some of which could actually exceed the SB in certain situations. These methods are the focus of the subsequent sections. Using the Intense (low-n) Lines of Hydrogenic Spectral SeriesIn hydrogen atoms and hydrogenlike ions (hereafter, hydrogenic atoms, for brevity), in spectral series, i.e., in radiative transitions between the upper states of various principal quantum number n and the fixed lower state of the principal quantum number n 0 , the most intense are the lines, corresponding to n = n 0 + 1 (α-line), n 0 + 2 (β-line), n 0 +3 (γ-line), n 0 +4 (δ-line) -in order of diminishing intensity. So, on the first glance, it seems that one should use the most intense lines, like the α-line or the β-line. However, there is a trade-off. The SB of the α-line is the smallest out of the spectral series. The SB increases along the spectral series: roughly speaking, as ∼n 2 for the ion broadening and ∼n 4 for the e...

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“…The Stark broadening is estimated 19 by quasicontiguous approximation 20 of the Holtsmark micro-field from the local electrons within the Debye radius, where the electron density is estimated by matching the quasicontiguous Stark width of the Lyman-a emission line from H atoms. A smaller electron density corresponds to a smaller Stark width, which results in narrower wings in the emission line profile and a sharper characteristic absorption dip in the center of the profile.…”

Section: à3mentioning

confidence: 99%