The abundance of boron and beryllium in alpha Lyrae

Boesgaard, Ann Merchant; Praderie, F.; Leckrone, D. S.; Faraggiana, R.; Hack, M.

doi:10.1086/181688

Cited by 8 publications

(7 citation statements)

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“…Vega was discovered to have the resonance line of B II at 1362 Å by Boesgaard et al (1974) with Copernicus observations at 0.2 Å resolution. The B/H abundance derived, with an estimate made for departures from local thermodynamic equilibrium, was 1.0ϫ10 Ϫ10 .…”

Section: Boronmentioning

confidence: 92%

“…There have been several recent studies of Be in halo stars: Gilmore, Edvardsson, and Nissen (1991), Gilmore et al (1992), Rebolo et al (1988), Ryan et al (1992), Boesgaard and King (1993), Garcia-Lopez et al (1995), a Keck Be project reported by , Thorburn and Hobbs (1996), Primas (1996), and Deliyannis et al (1997). All show an increase in Be in stars as the metallicity increases.…”

Section: Berylliummentioning

confidence: 99%

“…A survey of Be in solar-type stars was done by Boesgaard (1976) who found that while most such stars had normal (i.e., solar) Be, some of the hotter ones were deficient in Be. Boesgaard and King (1993) presented Be results for Li-normal, solar-metallicity stars and found a range in abundances of a factor of about three. A survey of Be in some 60 Li-deficient F and G dwarfs (Pop I) by shows Be deficiencies in the hotter stars, analogous to the Li dip at those temperatures, and near solar Be abundances for stars cooler than 6000 K. Stars in which both Li and Be are depleted but present in detectable amounts show a depletion pattern very close to the predictions of models by Pinsonneault, Kawalar, and Demarque (1990) of rotationally induced mixing.…”

Section: Berylliummentioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: Boronmentioning

confidence: 92%

Section: Berylliummentioning

confidence: 99%

Section: Berylliummentioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…They find that for six F and G main-sequence stars the average Be/H is 1.0 X 10" u , consistent with the value for the dwarfs in the field. The abundance of Be in Vega (type AO V) has been determined (Boesgaard et al 1974) to be 1.0 X 10" 11 also. This indicates that the same value for cosmic Be extends to the hotter main-sequence stars, i.e., that no temperature dependence exists.…”

Section: B Berylliummentioning

confidence: 97%

Stellar abundances of lithium, beryllium, and boron

Boesgaard¹

1976

PASP

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“….2 (z = 7o - 44) 13.4 (Z = 75 -79) 5.6 (Z = 80 -84) 6.1 (Z = 9O -94) of 2 higher than the average of all measured values, while S is about the same as the measurements in Cl meteorites. Table I is that of Boesgaard et al (1974) for Vega, while that in Fig. 1 is a modified meteoritic abundance (B = 350) given by Cameron (1973).…”

Section: Meteoritesmentioning

confidence: 99%