Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

Barklem, P. S.; O'Mara, B. J.

doi:10.1046/j.1365-8711.2000.03090.x

Cited by 59 publications

(39 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We estimated γ 6 using the Deridder & van Rensbergen (1976) approach with enhancement factor E = 1.5. In agreement with the conclusion of Mashonkina & Zhao (2006) we found that the recent calculations of the collisional damping constant made by Barklem & O'Mara (2000) overestimate γ 6 for this line by a factor 1.5. The near line wings are sensitive as well to the value of microturbulent velocity, while the line core is affected by the macroturbulence.…”

Section: One-dimensional Casesupporting

confidence: 91%

Modern solar facilities - advanced solar science

Kneer¹,

Puschmann²,

Wittmann³

2007

View full text Add to dashboard Cite

Section: One-dimensional Casesupporting

confidence: 91%

Modern solar facilities - advanced solar science

Kneer¹,

Puschmann²,

Wittmann³

2007

View full text Add to dashboard Cite

“…A striking excess of beryllium as compared with lithium is found in our Sun, since beryllium is rapidly destroyed by thermonuclear reactions at temperatures above 3.6 × 10 6 K, and its abundance also constraints on mixing between photospheric and deeper regions of stars, which is of particular interest in the Sun (Balachandran & Bell 1998). The surface contents of light elements, especially beryllium, provide information on nucleogenesis, and it almost relies on the Be II resonance doublet at 3130 Å, which emphasizes the importance of these lines in our present work (Barklem & O'Mara 2000). Moreover, Be II line profiles are of interest for opacity calculations (Dimitrijević & Sahal-Bréchot 1992).…”

Section: Introductionmentioning

confidence: 58%

“…Barklem & O'Mara 2000;Zethson et al 2001). Most recently, with the aid of these six Sr II lines, NLTE stellar strontium abundances have been derived by serval authors (Andrievsky et al 2011;Bergemann et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

Duan

Bari

et al. 2013

A&A

View full text Add to dashboard Cite

Aims. We present results of the electron-impact broadening parameters (i.e., widths and shifts) of spectral lines in singly ionized Be II, Sr II, and Ba II ions, calculated by using our relativistic quantum mechanical methods. Methods. In these calculations, Dirac R-matrix methods were used to solve (N + 1)-electron colliding systems to obtain the required scattering matrices. The dimensionless collision strength Ω(ε) is calculated as a function of incident electron energies ε.Results. The present line-broadening parameters are required for future spectral analysis by means of state-of-the-art nonlocal thermodynamic equilibrium atmospheres, which is now hampered largely by the paucity of reliable atomic and accurate line-broadening data tables. Our results for the spectral line-broadening parameters in the case of three ions obtained for a set of electron temperatures at an electron density 10 17 cm −3 show very good agreement with other theoretical calculations, and are much closer to the available experimental measurements.

show abstract

“…4.2.2). Whenever possible, we use damping constants as calculated by Anstee & O'Mara (1995), which have proved to be quite accurate (Anstee et al 1997;Barklem & O'Mara 2000).…”

Section: Abundance Analysis After Continuum Re-normalisation (Methods C)mentioning

confidence: 99%

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt¹,

Bikmaev

Catala

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract.One of the goals of the ground-based support program for the  and / satellite missions is to characterize suitable target stars for the part of the missions dedicated to asteroseismology. We present the detailed abundance analysis of nine of the potential  main targets using the semi-automatic software . For two additional  targets we could not perform the analysis due to the high rotational velocity of these stars. For five stars with low rotational velocity we have also performed abundance analysis by a classical equivalent width method in order to test the reliability of the  software. The agreement between the different methods is good. We find that it is necessary to measure abundances extracted from each line relative to the abundances found from a spectrum of the Sun in order to remove systematic errors. We have constrained the global atmospheric parameters T eff , log g, and [Fe/H] to within 70−100 K, 0.1−0.2 dex, and 0.1 dex for five stars which are slow rotators (v sin i < 15 km s −1 ). For most of the stars we find good agreement with the parameters found from line depth ratios, H α lines, Strömgren indices, previous spectroscopic studies, and also log g determined from the  parallaxes. For the fast rotators (v sin i > 60 km s −1 ) it is not possible to constrain the atmospheric parameters.

show abstract

Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

Cited by 59 publications

References 28 publications

Modern solar facilities - advanced solar science

Modern solar facilities - advanced solar science

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Contact Info

Product

Resources

About