Abundances and chemical stratification in the atmosphere of the HgMn star HD 175640

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dc.creatorThiam, M.
dc.creatorWade, G. A.
dc.creatorLeBlanc, F.
dc.creatorKhalack, V. R.
dc.date2006-12-12
dc.date.accessioned2026-07-07T06:34:40Z
dc.date.available2026-07-07T06:34:40Z
dc.descriptionWe present the results of a study of the photospheric abundances of the HgMn star HD 175640, conducted using archival ESO-UVES spectra. A large number of unblended (titanium, chromium, manganese and iron) lines were studied to search for the presence of chemical stratification in the atmosphere of this star. The selected lines are located in the visible region of the spectrum, longward of the Balmer jump, in orders with S/N $\geq$ 300. We derived the abundance of each element by calculating independently the abundance associated each line. We then characterized the depth of formation of each line, and examined the dependence of abundance on optical depth. Titanium, chromium, manganese and iron show no variation of their abundance with optical depth. These four elements do not appear to be strongly stratified in the atmosphere of HD 175640. This indicates that if stratification occurs, it must be in atmospheric layers which are not diagnosed by the spectral lines studied, or that it is too weak to detect using these data. We also report evidence that HD 175640 is an SB1, and furthermore report anomalous shifts of some strong Fe {\sc II} lines, the origin of which is unclear.
dc.description6 pages, 4 figures, Accepted in the proceedings of the 2006 conference "Stellar Magnetic Fields", Special Astrophysical Observatory of the Russian Academy of Sciences, Aug. 28 - Sept. 1 2006
dc.identifierhttps://arxiv.org/abs/astro-ph/0612323
dc.identifierhttp://arxiv.org/abs/astro-ph/0612323
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/99595
dc.subjectAstrophysics
dc.titleAbundances and chemical stratification in the atmosphere of the HgMn star HD 175640
dc.typetext

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