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arXiv · 1010.0003

The Structure of the {\beta} Leonis Debris Disk

Nathan D. Stock·Kate Y. L. Su·Wilson Liu·Phil M. Hinz·George H. Rieke·Massimo Marengo·Karl R. Stapelfeldt·Dean C. Hines·David E. Trilling
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Abstract

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.

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Nathan D. Stock, Kate Y. L. Su, Wilson Liu, Phil M. Hinz, George H. Rieke, Massimo Marengo, Karl R. Stapelfeldt, Dean C. Hines, David E. Trilling. 2010-09-30. The Structure of the {\beta} Leonis Debris Disk. https://doi.org/10.1088/0004-637x/724/2/1238

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