Modeling the Infrared Emission from the Epsilon Eridani Disk

Details Modeling the Infrared Emission from the Epsilon Eridani Disk Modeling the Infrared Emission from the Epsilon Eridani Disk

2003-11-04

arxiv.org/abs/astro-ph/0311069v1

Astrophys.J. 598 (2003) L51-L54

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

10.1086/380495

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.

Affiliated with

Also associated with

No associations

Rating

Modeling the Infrared Emission from the Epsilon Eridani Disk does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Modeling the Infrared Emission from the Epsilon Eridani Disk, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Modeling the Infrared Emission from the Epsilon Eridani Disk will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-264198