The structure of the β leonis debris disk

Abstract

We combine nulling interferometry at 10 μm using the MMT and Keck Telescopes with spectroscopy, imaging, and photometry from 3 to 100 μm using Spitzer to study the debris disk around β 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 β 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 2-3 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, β Leo lacks a dominant outer belt near 100 AU. © 2010. The American Astronomical Society.