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The Dust in β Pictoris Systems

Published online by Cambridge University Press:  27 February 2018

S.B. Fajardo-Acosta
S.B. Fajardo-Acosta*
Affiliation:
Penn State Erie, Division of Science, Station Road, Erie, PA 16563

Abstract

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The bright 10 μm excess emission of β Pic stars allows detailed spectroscopy of their warm circumstellar solid material. The silicate features in β Pic and 51 Oph are broader and contain more structure than interstellar and most circumstellar emission features. The β Pic and 51 Oph features are remarkably similar to those in comets Halley, Bradfield 1987s, Levy 1990 XX, and Mueller 1993a which have 11.3 μm emission features characteristic of crystalline silicates. In contrast, other β Pic-type stars (ζ Lep and β UMa) show weak 10 μm emission from larger, amorphous dust grains. Some comets such as Austin 1990 V emit similar weak 10 μm features.

Type
XIII. Relationships to Interstellar Dust
Information
International Astronomical Union Colloquium , Volume 150: Physics, Chemistry and Dynamics of Interplanetary Dust , 1996 , pp. 507 - 512
Copyright
Copyright © Astronomical Society of the Pacific 1996

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