The Structure of the β Leonis Debris Disk

Details The Structure of the β Leonis Debris Disk The Structure of the β Leonis Debris Disk

2010-09-30

arxiv.org/abs/1010.0003v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

14 page body, 3 page appendix, 15 figures

Scientific paper

We combine nulling interferometry at 10 {\mu}m using the MMT and Keck Telescopes with spectroscopy, imaging, and photometry from 3 to 100 {\mu}m using Spitzer to study the debris disk around {\beta} Leo over a broad range of spatial scales, corresponding to radii of 0.1 to ~100 AU. We have also measured the close binary star o Leo with both Keck and MMT interferometers to verify our procedures with these instruments. The {\beta} Leo debris system has a complex structure: 1.) relatively little material within 1 AU; 2.) an inner component with a color temperature of ~600 K, fitted by a dusty ring from about 2 to 3 AU; and 3.) a second component with a color temperature of ~120 K fitted by a broad dusty emission zone extending from about ~5 AU to ~55 AU. Unlike many other A-type stars with debris disks, {\beta} Leo lacks a dominant outer belt near 100 AU.

Affiliated with

Also associated with

No associations

Rating

The Structure of the β Leonis Debris 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 The Structure of the β Leonis Debris Disk, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Structure of the β Leonis Debris Disk will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-326891