The Chemical Composition of Alpha Centauri A: Strong Lines and the ABO Theory of Collisional Line Broadening

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dc.creatorDoyle, Marianne T.
dc.creatorO'Mara, B. J.
dc.creatorRoss, J. E.
dc.creatorBessell, M. S.
dc.date2004-07-22
dc.date.accessioned2026-07-07T10:27:15Z
dc.date.available2026-07-07T10:27:15Z
dc.descriptionThe mean abundances of Mg, Si, Ca, Ti, Cr and Fe based on both strong and weak lines of Alpha Centauri A are determined by matching the observed line profiles with those synthesized from stellar atmospheric models and comparing these results with a similar analysis for the Sun. There is good agreement between the abundances from strong and weak lines. Strong lines should generally be an excellent indicator of abundance and far easier to measure than the weak lines normally used. Until the development of the Anstee, Barklem and O'Mara theory for collisional line broadening, the uncertainty in the value of the damping constant prevented strong lines being used for abundance determinations other than in close differential analyses. We found that Alpha Centauri A has a mean overabundance of 0.12+/-0.06 dex compared to solar mean abundances. This result agrees remarkably well with previous studies that did not use strong lines or the Anstee, Barklem and O'Mara theory for collisional line broadening. Our result support the conclusion that reliable abundances can be derived from strong lines provided this new theory for line broadening is used to calculate the van der Waal's damping.
dc.description8 pages, 3 figures, accepted for publication in PASA. B. J. O'Mara is deceased
dc.identifierhttps://arxiv.org/abs/astro-ph/0407468
dc.identifierhttp://arxiv.org/abs/astro-ph/0407468
dc.identifierPubl.Astron.Soc.Austral.22:6-12,2005
dc.identifierdoi:10.1071/AS03054
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177101
dc.subjectAstrophysics
dc.titleThe Chemical Composition of Alpha Centauri A: Strong Lines and the ABO Theory of Collisional Line Broadening
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