Stark Broadening of F III Lines in Laboratory and Stellar Plasma

Abstract

∨ ic ′ a UDC 533.9.082.5Using a semiclassical approach, we have considered electron-, proton-, and ionized helium-impact line widths and shifts for the F III 2p 3 4 S o -3s 4 P resonant line. Moreover, for 10 F III multiplets where the full semiclassical perturbation approach is not applicable in an adequate way due to the lack of reliable atomic data, electron-impact line widths have been calculated within the modified semiempirical approach. Results are obtained as a function of temperature for perturber density of 10 17 cm -3 . The theoretical data obtained have been used to consider the influence of Stark broadening for A-type star atmosphere conditions.

Stark Parameter Regularities of Multiply Charged Ion Spectral Lines Originating from the Same Transition Array

“…Using theoretical and experimental Stark width data published so far (see, e.g., Purić & Š ćepanović 1999;Š ćepanović & Purić 2003;Griem 1974;Konjević et al 1984Konjević et al , 2002Konjević & Wiese 1990, and references therein;Dimitrijević & Sahal-Brechot 1994, 1998a, 1998b, 1998c, 1998d, 1998e, 1999, 2000Milosavljevic et al 2001;Srećković et al 2001;Ralchenko et al 2003;Ben Nessib et al 2004;Ivković et al 2005;Elabidi et al 2005;Simic et al 2005), we have obtained the reduced w à dependence on the inverse value of the upper level ionization potential normalized to electron density N e ¼ 10 23 m À3 and using equation (4) to an electron temperature T ¼ 10 5 K, as it is presented in Figures 1a, 1b, and 1c. The reduced Stark width theoretical ( Fig.…”

“…Using this equation one can calculate the Stark width of a particular spectral line for different electron densities and temperatures. In order to get FWHM in the wavelength units (nm), the electron density has to be taken in m À3 and electron temperature in K. The studied regularities of the Stark width of spectral lines, which originate from the 3s-3p transition data published so far ( Konjević et al 1984( Konjević et al , 2002Konjević & Wiese 1990;Purić & Š ćepanović 1999;Š ćepanović & Purić 2003;Ivković et al 2005;Dimitrijević & Sahal-Brechot 1994, 1998a, 1998b, 1998c, 1998d, 1998e, 1999, 2000Ralchenko et al 2003;Milosavljevic et al 2001;Elabidi et al 2005;Simic et al 2005;Srećković et al 2001;Ben Nessib et al 2004), enabled these predictions with the average accuracy of the data used in establishing Stark width dependence on the upper level ionization potential and rest core charge of the emitter. This is in accordance with the conclusions drawn in reviews (see, e.g., Konjević et al 1984Konjević et al , 2002Konjević & Wiese 1990), where the experimental and theoretical data are critically evaluated.…”

Stark Broadening of Neutral Boron Lines

“…In astrophysics, Stark broadening data for various atomic and ionic lines are of particular interest for white dwarfs, where this line broadening mechanism is usually the principal one [1][2][3][4][5][6][7][8]. This broadening mechanism may be of interest for the main sequence stars, especially for A type and late B type [9][10][11][12][13][14][15][16][17][18][19]. It could be mentioned the increasing astrophysical importance of Stark broadening data for various atoms and ions of trace elements.…”

Stark widths of Sc IV spectral lines within 4s-4p transition array

“…In atmospheres of white dwarfs, pre white dwarf stars, and post AGB(Asymptotic Giant Branch) stars this is usually the main broadening mechanism (Tankosić et al, 2003;Milovanović et al, 2004;Simić et al, 2006;Dufour et al, 2011). It can not be neglected and in some atmospheric layers of A and late B stars (Simić et al, 2005b(Simić et al, ,a, 2009. As an example, have shown that, for A-type star atmospheres, the inclusion of Stark broadening can change the equivalent widths by 10-45%.…”