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Lambda Boo Abundance Patterns: Accretion from Orbiting Sources
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The abundance anomalies in lambda Boo stars are popularly explained by element-specific mass inflows at rates that are much greater than empirically-inferred bounds for interstellar accretion. Therefore, a lambda Boo star's thin outer envelope must derive from a companion star, planet, analogs to Kuiper Belt Objects or a circumstellar disk. Because radiation pressure on gas-phase ions might selectively allow the accretion of carbon, nitrogen, and oxygen and inhibit the inflow of elements such as iron, the source of the acquired matter need not contain dust. We propose that at least some lambda Boo stars accrete from the winds of hot Jupiters.
Forward citations
Cited by 2 Pith papers
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Discovery of the $\lambda$ Bootis phenomenon in an early B-type star
HD 37356, a B2 IV star, shows depleted refractory elements and normal volatiles, making it the first known early B-type Lambda Bootis star.
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Is the composition of the Solar atmosphere unusual, and if so, why? Possible interpretations
A review of the 10-20% solar volatile-to-refractory excess relative to solar twins, weighing galactic, protoplanetary, and planetary-ingestion explanations and finding no decisive answer.
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