Modeling the Infrared Emission from the Epsilon Eridani Disk
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 90% is also successful in reproducing the IR to submillimeter dust emission spectral energy distribution as well as the 850μm flux radial profile of the dust ring around the more evolved MS star Epsilon Eridani. Predictions are made for future SIRTF observations which may allow a direct test of the porous dust model.
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