On the origin of the light elements (<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>Z</mml:mi><mml:mo>&lt;</mml:mo><mml:mn /><mml:mn>6</mml:mn><mml:mn /></mml:math>)

Reeves, Hubert

doi:10.1103/revmodphys.66.193

Cited by 189 publications

(94 citation statements)

References 102 publications

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“…Be is mainly produced by spallation reactions in the interstellar medium, while it is burned in the hot stellar furnaces (e.g. Reeves 1994). While most works of light element abundances are based on Li (the abundances of this element are easier to measure), Be studies have one major advantage when compared with Li.…”

Section: Introductionmentioning

confidence: 99%

Beryllium abundances in stars hosting giant planets

Santos¹,

López²,

Israelian³

et al. 2002

A&A

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Abstract.We have derived beryllium abundances in a wide sample of stars hosting planets, with spectral types in the range F7V−K0V, aimed at studying in detail the effects of the presence of planets on the structure and evolution of the associated stars. Predictions from current models are compared with the derived abundances and suggestions are provided to explain the observed inconsistencies. We show that while still not clear, the results suggest that theoretical models may have to be revised for stars with T eff < 5500 K. On the other hand, a comparison between planet host and non-planet host stars shows no clear difference between both populations. Although preliminary, this result favors a "primordial" origin for the metallicity "excess" observed for the planetary host stars. Under this assumption, i.e. that there would be no differences between stars with and without giant planets, the light element depletion pattern of our sample of stars may also be used to further investigate and constraint Li and Be depletion mechanisms.

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Section: Introductionmentioning

confidence: 99%

Beryllium abundances in stars hosting giant planets

Santos¹,

López²,

Israelian³

et al. 2002

A&A

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“…Other ideas (e.g. Prantzos et al 1993) were only partially successful in that respect (see Reeves 1994 for a summary of the situation in the mid-90ies). Ramaty et al (1997) showed that a metallicity-independent GCR composition is the only viable alternative for energetic reasons: if in the early Galaxy GCR had a metallic content much lower than today, they would need much more energy than supernovae can provide to always yield primary Be.…”

Section: Introductionmentioning

confidence: 99%

Production and evolution of Li, Be, and B isotopes in the Galaxy

Prantzos

2012

A&A

169

159

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Context. We reassess the problem of the production and evolution of the light elements Li, Be and B and of their isotopes in the Milky Way in the light of new observational and theoretical developments. Aims. The main novelty is the introduction of a new scheme for the origin of Galactic cosmic rays (GCR), which for the first time enables a self-consistent calculation of their composition during galactic evolution. Methods. The scheme accounts for key features of the present-day GCR source composition, it is based on the wind yields of the Geneva models of rotating, mass-losing stars and it is fully coupled to a detailed galactic chemical evolution code. Results. We find that the adopted GCR source composition accounts naturally for the observations of primary Be and helps understanding why Be follows Fe more closely than O. We find that GCR produce ∼70% of the solar 11 B/ 10 B isotopic ratio; the remaining 30% of 11 B presumably result from ν-nucleosynthesis in massive star explosions. We find that GCR and primordial nucleosynthesis can produce at most ∼30% of solar Li. At least half of the solar Li has to originate in low-mass stellar sources (red giants, asymptotic giant branch stars, or novae), but the required average yields of those sources are found to be much higher than obtained in current models of stellar nucleosynthesis. We also present radial profiles of LiBeB elemental and isotopic abundances in the Milky Way disc. We argue that the shape of those profiles -and the late evolution of LiBeB in general -reveals important features of the production of those light elements through primary and secondary processes.

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“…Boron in diffuse interstellar clouds is also 11 B-rich ( 11 B/ 10 B = 3.4 AE 0.7, Lambert et al 1998) relative to GCR. This 11 B enrichment has been proposed to result from the addition of B made by low-energy spallation which would be enriched in 11 B according to predictions made from available cross sections (Reeves 1994) and/or to the addition of B made by neutrino-induced spallation of C in type II ▶ supernovae (Lambert et al 1998). These processes are likely to operate at galactic time scales but irradiation processes around the young forming Sun also produced a fraction of the Solar System boron.…”

Section: See Alsomentioning

confidence: 99%

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Rouan¹

2015

Encyclopedia of Astrobiology

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On the origin of the light elements (Z<6)

Cited by 189 publications

References 102 publications

Beryllium abundances in stars hosting giant planets

Beryllium abundances in stars hosting giant planets

Production and evolution of Li, Be, and B isotopes in the Galaxy

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