Pressure Broadening and Solar Limb Effect

Vince, I.; Dimitrijević, M. S.; Kršljanin, V.

doi:10.1007/978-94-009-5372-7_30

Cited by 12 publications

(7 citation statements)

References 6 publications

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“…The second significant feature is the relatively good agreement between the present results and both SCP theory [35] and Sahal-Bréchot predictions in [28]-labelled as 'SB' in the figure 7 caption. However, the present measured values for multiplet (2), λ = 634.7 and 637.1 nm, as well as those from [29], are notably lower than predicted by semi-classical theories. Quantum mechanical calculations based on the distorted-wave approximation, including configuration mixing done by Blaha in [30], are in close agreement with our experimental results for this multiplet (the agreement is also very close for multiplet (1), λ = 385.4, 385.6 and 386.3 nm).…”

Section: Results and Conclusioncontrasting

confidence: 86%

“…In atmospheres of such stars Stark broadening is the dominant pressure-broadening mechanism and the knowledge of the Stark parameters is very important for a number of astrophysical problems. Even in atmospheres of relatively cool stars such as the Sun, where line broadening caused by collisions with neutrals is dominant, Stark broadening may compete with other broadening mechanisms in the line wings [2]. Stark broadening of spectral lines has also been attracting new interest in astrophysics [3], owing to the development of research on the physics of stellar interiors: in subphotospheric envelopes, the energy transport models require knowledge of radiative opacities and thus the relevant atomic process must be known with accuracy.…”

Section: Introductionmentioning

confidence: 99%

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Stark broadening and shift measurements of visible Si II lines

González¹,

Aparicio²,

Val

et al. 2002

J. Phys. B: At. Mol. Opt. Phys.

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A set of experimental Stark width and shift parameters of visible singly ionized silicon spectral lines is reported in this paper. Measurements have been made on a pulsed plasma generated in a linear discharge lamp filled with a mixture of silane and helium. Electron density and temperature in this plasma range from 0.2 to 0.9 × 1023 m−3 and from 16 000 to 20 000 K respectively. Electron density has been simultaneously determined by two-wavelength interferometry and from Stark broadening of He I 501.6 nm, He I 728.1 nm and Hα lines. Temperature has been simultaneously determined from a Boltzmann plot of He I lines, from absolute emission of He I lines and from a Boltzmann plot of Si II lines. Dependences of measured Stark parameters on electron density and temperature have been investigated and the final results have been compared with most of the previous experimental data as well as with some theoretical models.

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Section: Results and Conclusioncontrasting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Stark broadening and shift measurements of visible Si II lines

González¹,

Aparicio²,

Val

et al. 2002

J. Phys. B: At. Mol. Opt. Phys.

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“…Moreover, Stark broad ening of lines orginating from energy levels with high prin cipal quantum numbers may be important and for some lines in atmospheres of cooler stars (see e.g. Vince et al 1985).…”

Section: Introductionmentioning

confidence: 99%

Stark widths for astrophysically important ns-np transitions in Sc II, Y II and Zr II spectra

Dimitrijević

1996

Astron. Astrophys. Suppl. Ser.

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“…This broadening mechanism also may be important in the case of cooler stars, e.g. solar type stars, for transitions involving higher principal quantum numbers (Vince et al 1985). An interesting application where such a mechanism is of interest is also the modeling and investigation of subphotospheric layers (Seaton 1987).…”

Section: Introductionmentioning

confidence: 99%

The electron-impact broadening parameters for Co III spectral lines

Tankosic

Popović

Dimitrijević

2003

A&A

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Abstract. In hot star atmospheres, the Stark broadening mechanism is the main pressure broadening mechanism. An interesting application where such a mechanism is of interest is the modeling and investigation of hot star spectra, stellar atmospheres and subphotospheric layers. Consequently, for the investigation and modeling of the Hg-Mn star and other type of hot star atmospheres, the Stark broadening parameters for Co III spectral lines may be of interest.Here we present Stark broadening data for 20 Co III spectral lines (from a 6 D -z 6 D o and a 6 D -z 6 F o Co III multiplets), as a function of temperature, calculated by using the modified semi-empirical approach. The importance of the electron-impact effect in the case of the Co III 194.98 nm line for several stellar atmosphere models has been tested.

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Pressure Broadening and Solar Limb Effect

Cited by 12 publications

References 6 publications

Stark broadening and shift measurements of visible Si II lines

Stark broadening and shift measurements of visible Si II lines

Stark widths for astrophysically important ns-np transitions in Sc II, Y II and Zr II spectra

The electron-impact broadening parameters for Co III spectral lines

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