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Light-element abundances of peculiar a stars

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Abstract

Light-element abundances are compiled for six peculiar A stars (3 CenA, α2 CVn, HR 1732,v For, κ Cnc, and 112 Her) with Heilines very weak for their colours. The abundances are interpreted on the theory that peculiar A stars were once secondaries in binary systems in which the primaries exploded as type II supernovae. During the explosions of the primaries, protons were accelerated to high energies (>20 MeV) in shock waves at the secondaries, and spallation of He, C, N, and O occurred. This was followed by the arrival of heavier elements from the primaries. Abundances on α2 CVn, HR 1732, andv For were subsequently modified by surface nuclear reactions involving protons and α-particles accelerated to lower energies (∼10 MeV), probably by magnetic fields. Successive (α, γ) reactions formed Si28 from Ne20, and (p, α) reactions acting on A40 and Ca40 may have contributed to the excesses of Cl observed on α2 CVn and HR 1732. These proposals have interesting implications with regard to the relative abundances of the iron-peak elements found on peculiar A stars and in the Solar System.

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  1. Royal Observatory, Edinburgh, Scotland

    B. N. G. Guthrie

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  1. B. N. G. Guthrie
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Guthrie, B.N.G. Light-element abundances of peculiar a stars. Astrophys Space Sci 8, 172–184 (1970). https://doi.org/10.1007/BF00650879

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  • DOI: https://doi.org/10.1007/BF00650879

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