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Warm dust around ϵ Eridani

Published online by Cambridge University Press:  10 November 2011

Martin Reidemeister ,
Alexander V. Krivov ,
Christopher C. Stark ,
Jean-Charles Augereau ,
Torsten Löhne  and
Sebastian Müller
Martin Reidemeister
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: martin.reidemeister@astro.uni-jena.de
Alexander V. Krivov
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: martin.reidemeister@astro.uni-jena.de
Christopher C. Stark
Affiliation:
Department of Physics, University of Maryland, Box 197, 082 Regents Drive, College Park, MD 20742-4111, USA
Jean-Charles Augereau
Affiliation:
Laboratoire d'Astrophysique de Grenoble, CNRS UMR 5571, Université Joseph Fourier, Grenoble, France
Torsten Löhne
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: martin.reidemeister@astro.uni-jena.de
Sebastian Müller
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: martin.reidemeister@astro.uni-jena.de
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Abstract

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ϵ Eridani hosts one known inner planet and an outer Kuiper belt analog. Further, Spitzer/IRS measurements indicate that warm dust is present at distances as close as a few AU from the star. Its origin is puzzling, since an “asteroid belt” that could produce this dust would be unstable because of the inner planet. We tested a hypothesis that the observed warm dust is generated by collisions in the outer belt and is transported inward by P-R drag and strong stellar winds. With numerical simulation we investigated how the dust streams from the outer ring into the inner system, and calculated the thermal emission of the dust. We show that the observed warm dust can indeed stem from the outer belt. Our models reproduce the shape and magnitude of the observed SED from mid-IR to sub-mm wavelengths, as well as the Spitzer/MIPS radial brightness profiles.

Keywords

stars: individual (ϵ Eridani)planetary systemsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 455 - 456
Copyright
Copyright © International Astronomical Union 2011

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