Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7193
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dc.contributor.authorPandey, G-
dc.contributor.authorLambert, D. L-
dc.date.accessioned2017-10-11T10:22:34Z-
dc.date.available2017-10-11T10:22:34Z-
dc.date.issued2017-10-01-
dc.identifier.citationThe Astrophysical Journal, Vol. 847, No. 2, 127en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/7193-
dc.descriptionRestricted Accessen_US
dc.description.abstractOptical high-resolution spectra of V652 Her and HD 144941, the two extreme helium stars with exceptionally low C/He ratios, have been subjected to a non-LTE abundance analysis using the tools TLUSTY and SYNSPEC. Defining atmospheric parameters were obtained from a grid of non-LTE atmospheres and a variety of spectroscopic indicators including He i and He ii line profiles, and the ionization equilibrium of ion pairs such as C ii/C iii and N ii/N iii. The various indicators provide a consistent set of atmospheric parameters: T eff = 25,000 ± 300 K, log g = 3.10 ± 0.12(cgs), and ξ = 13 ± 2 km s−1 are provided for V652 Her, and T eff = 22,000 ± 600 K, log g = 3.45 ± 0.15 (cgs), and ξ = 10 km s−1 are provided for HD 144941. In contrast to the non-LTE analyses, the LTE analyses—LTE atmospheres and an LTE line analysis—with the available indicators do not provide a consistent set of atmospheric parameters. The principal non-LTE effect on the elemental abundances is on the neon abundance. It is generally considered that these extreme helium stars with their very low C/He ratio result from the merger of two helium white dwarfs. Indeed, the derived composition of V652 Her is in excellent agreement with predictions by Zhang & Jeffery, who model the slow merger of helium white dwarfs; a slow merger results in the merged star having the composition of the accreted white dwarf. In the case of HD 144941, which appears to have evolved from metal-poor stars, a slow merger is incompatible with the observed composition but variations of the merger rate may account for the observed composition. More detailed theoretical studies of the merger of a pair of helium white dwarfs are to be encouraged.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/aa88bb-
dc.rights© The American Astronomical Society-
dc.subjectStars: abundancesen_US
dc.subjectStars: atmospheresen_US
dc.subjectStars: chemically peculiaren_US
dc.subjectStars: evolutionen_US
dc.subjectStars: fundamental parametersen_US
dc.titleNon-local Thermodynamic Equilibrium Abundance Analyses of the Extreme Helium Stars V652 Her and HD 144941en_US
dc.typeArticleen_US
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