Abundances of the Light Elements in the Hydrogen-Poor Star HD 30353

Wallerstein, George; Greene, T. F.; Tomley, L.

doi:10.1086/149326

Cited by 19 publications

(10 citation statements)

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“…The enhanced F abundances (see Figure 4) in cool EHes are evidence of nucleosynthesis in their earlier evolution. The abundances for the other elements presented in Figure 4 are adopted from Pandey et al (2001) for FQ Aqr, LS IV-14 • 109, BD -1 • 3438, and LS IV-1 • 2, from Pandey & Reddy (2006) for LSS 3378, and from Wallerstein, Greene & Tomley (1967) and Pandey et al (2006b) for KS Per. The F, C, and O abundances in cool EHes are independent of the star's initial metallicity (Fe abundance); the N abundances, however, show a clear trend with Fe (see Figure 4).…”

Section: Discussionmentioning

confidence: 99%

“…At the bottom, KS Per is added, which is known to be H-deficient (Wallerstein, Greene & Tomley 1967;Pandey et al 2006b). The spectrum of KS Per very much resembles the spectrum of the cool EHe LS IV-14 • 109, except for the C i lines which are extremely week or not present in the KS Per's spectrum (Wallerstein, Greene & Tomley 1967;Pandey et al 2006b). Singly ionized metal lines (particularly Fe ii) are identified as contributor to a stellar line at or about F i lines in KS Per's spectrum.…”

Section: F I Linesmentioning

confidence: 99%

“…All spectra are alligned to the rest wavelengths of the well known lines, that fall in the wavelength regions. At the bottom, KS Per is added, which is known to be H-deficient (Wallerstein, Greene & Tomley 1967;Pandey et al 2006b). The spectrum of KS Per very much resembles the spectrum of the cool EHe LS IV-14 • 109, except for the C i lines which are extremely week or not present in the KS Per's spectrum (Wallerstein, Greene & Tomley 1967;Pandey et al 2006b).…”

Section: F I Linesmentioning

confidence: 99%

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The Discovery of Fluorine in Cool Extreme Helium Stars

Pandey

2006

ApJ

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Neutral fluorine (F i) lines are identified in the optical spectra of cool EHe stars. These are the first identification of F i lines in a star's spectrum, and provide the first measurement of fluorine abundances in EHe stars. The results show that fluorine is overabundant in EHe stars. The overabundance of fluorine provides evidence for the synthesis of fluorine in these stars, that is discussed in the light of asymptotic giant branch (AGB) evolution, and the expectation from accretion of an He white dwarf by a C-O white dwarf.

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Section: Discussionmentioning

confidence: 99%

Section: F I Linesmentioning

confidence: 99%

Section: F I Linesmentioning

confidence: 99%

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The Discovery of Fluorine in Cool Extreme Helium Stars

Pandey

2006

ApJ

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“…Early estimates of chemical composition of KS Per by Wallerstein et al (1967) and Nariai (1967) showed that the atmosphere is very hydrogen-poor H/He≈ 10 −4 (by number). The abundance of carbon compared to that of nitrogen is also low.…”

Section: Model Atmospheresmentioning

confidence: 99%

Improved parameters of the hydrogen-deficient binary star KSPer

Kipper,

Klochkova

2008

Preprint

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Using the high resolution spectra secured with the Nasmyth Echelle Spectrograph NES of the 6 meter telescope we analysed the hydrogen-deficient binary star KS Per. The atmospheric parameters derived are: T eff = 9500±300 K, log g = 2.0±0.5, and ξ t = 9.5±0.5 km s −1 . The hydrogen deficiency is H/He = 3•10 −5 , iron abundance is reduced by 0.8 dex, nitrogen abundance is very high [N/Fe] = 1.4, but carbon and oxygen abundances are low. The star luminosity is log L/L ⊙ = 3.3. A complex absorption and emission structure of the Na I D doublet was revealed. We suggest that the emission component forms in the circumbinary gaseous envelope.

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“…Table 1 lists the abundance determinations in 3 Lyr. Balachandran et al 1960Balachandran et al 1961Balachandran et al 1965Balachandran et al 1977Balachandran et al 1979Balachandran et al 1980Balachandran et al 1982Balachandran et al 1986 As for KS Per, which also does not display a Balmer discontinuity Danziger et al (1967) and Wallerstein et al (1967) compared fluxes and profiles with those suggested by Bohm-Vitense's H-poor model atmosphere calculations and derived -4 a value of the ratio of H over He of the order of 10 , and a high abundance of N relative to C and to 0.…”

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confidence: 90%

Evolution Diagnostics in Interacting Binaries

Sahade

1988

International Astronomical Union Colloquium

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Through the analysis and interpretation of observational material, particularly on the part of Otto Struve and his collaborators, the structure of an interacting binary is depicted (cf. Sahade and Wood 1978) as formed by a) the two stellar components; b) a gaseous stream from the less massive and more evolved component of the system towards the companion; c) a circumstellar gaseous envelope –designated as “ring” or “disk” depending on the density of the material; d) a circumbinary gaseous envelope that surrounds the whole system and is normally in expansion, as suggested by the conventional, ground–based observations.The evolution of interacting binaries involves the effect of matter outflow and transfer in at least a stage of rapid mass loss and a stage of slow mass loss. As a result, the evolution of the components appreciably departs from the evolution of single stars and produces very bizarre objects which find no counterparts among non-binaries. Both the observational and the computational results suggest that the amount of mass involved in the process of mass outflow must be a large percentage of the total mass of the evolving component. It seems, therefore, reasonable to expect to find evidence, in evolved systems, for processed material from the interior of the mass-losing component.

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Abundances of the Light Elements in the Hydrogen-Poor Star HD 30353

Cited by 19 publications

References 0 publications

The Discovery of Fluorine in Cool Extreme Helium Stars

The Discovery of Fluorine in Cool Extreme Helium Stars

Improved parameters of the hydrogen-deficient binary star KSPer

Evolution Diagnostics in Interacting Binaries

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