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 $\beta$ 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.

To appear in The Astrophysical Journal Letters (2003-November-20th issue); 11 pages; 2 figures

References in corpus (2)

• Modeling the Infrared Emission from the HD 141569A Disk
• Modeling the Infrared Emission from the HR 4796A Disk

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• Hubble and Spitzer Space Telescope Observations of the Debris Disk around the Nearby K Dwarf HD 92945
• Gas lines from the 5-Myr old optically thin disk around HD141569A. Herschel observations and modeling
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• The Dynamical Influence of a Planet at Semimajor Axis 3.4 AU on the Dust Around Epsilon Eridani
• A Spitzer/IRAC Search for Substellar Companions of the Debris Disk Star epsilon Eridani
• Limits on the Optical Brightness of the Epsilon Eridani Dust Ring
• SIMBA's view of the epsilon Eri disk
• Light Scattering and Thermal Emission by Primitive Dust Particles in Planetary Systems
• Collisional parameters of planetesimal belts, precursor of debris disks, perturbed by a nearby giant planet