Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-23T14:29:36.639Z Has data issue: false hasContentIssue false

Warm dust around ϵ Eridani

Published online by Cambridge University Press:  10 November 2011

Martin Reidemeister
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: [email protected]
Alexander V. Krivov
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: [email protected]
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: [email protected]
Sebastian Müller
Affiliation:
Astrophysikalisches Institut, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Backman, D., Marengo, M., Stapelfeldt, K., et al. 2009, ApJ, 690, 1522Google Scholar
Benedict, G. F., McArthur, B. E., Gatewood, G., et al. 2006, AJ, 132, 2206Google Scholar
Brogi, M., Marzari, F., & Paolicchi, P. 2009, A&A, 499, L13Google Scholar
Butler, R. P., Wright, J. T., Marcy, G. W., et al. 2006, ApJ, 646, 505CrossRefGoogle Scholar
Greaves, J. S., Holland, W. S., Wyatt, M. C., et al. 2005, ApJL, 619, L187Google Scholar
Hatzes, A. P., Cochran, W. D., McArthur, B., et al. 2000, ApJL, 544, L145Google Scholar
Krivov, A. V., Löhne, T., & Sremčević, M. 2006, A&A, 455, 509Google Scholar
Laor, A. & Draine, B. T. 1993, ApJ, 402, 441CrossRefGoogle Scholar
Li, A. & Greenberg, J. M. 1998, A&A, 331, 291Google Scholar
Wood, B. E., Müller, H.-R., Zank, G. P., & Linsky, J. L. 2002, ApJ, 574, 412CrossRefGoogle Scholar