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Modeling the Infrared Emission from the epsilon Eridani Disk

Aigen Li et al 2003 ApJ 598 L51-L54   doi: 10.1086/380495  Help

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Aigen Li1, J. I. Lunine1 and G. J. Bendo1
1 Theoretical Astrophysics Program, Steward Observatory and Lunar and Planetary Laboratory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721
E-mail: agli@lpl.arizona.edu, jlunine@lpl.arizona.edu and gbendo@as.arizona.edu

ABSTRACT. We model the infrared (IR) emission from the ringlike dust disk around the main-sequence (MS) star epsilon Eridani, a young analog to our solar system, in terms of a porous dust model previously developed for the extended wedge-shaped disk around the MS star β Pictoris and the sharply truncated ringlike disks around the Herbig Ae/Be stars HR 4796A and HD 141569A. It is shown that the porous dust model with a porosity of ~90% is also successful in reproducing the IR to submillimeter dust emission spectral energy distribution as well as the 850 μm flux radial profile of the dust ring around the more evolved MS star epsilon Eri. Predictions are made for future SIRTF observations that may allow a direct test of the porous dust model.

Subject headings: circumstellar matter; dust, extinction; infrared: stars; planetary systems: protoplanetary disks; stars: individual (epsilon Eridani)

Print publication: Issue 1 (2003 November 20)
Received 2003 June 27, accepted for publication 2003 October 8
Published 2003 October 31

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