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Modeling the Infrared Emission from the Epsilon Eridani Disk

Aigen Li·J. I. Lunine·G. J. Bendo
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Abstract

We model the infrared (IR) emission from the ring-like 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 ring-like disks around the Herbig Ae/Be stars HR 4796A and HD 141569A. It is shown that the porous dust model with a porosity of $\simali$90% is also successful in reproducing the IR to submillimeter dust emission spectral energy distribution as well as the 850$\mum$ flux radial profile of the dust ring around the more evolved MS star Epsilon Eridani. Predictions are made for future {\it SIRTF} observations which may allow a direct test of the porous dust model.

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Aigen Li, J. I. Lunine, G. J. Bendo. 2003-11-04. Modeling the Infrared Emission from the Epsilon Eridani Disk. https://doi.org/10.1086/380495

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