The structure of the β 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

doi:10.1088/0004-637X/724/2/1238

The structure of the β 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

Astronomy and Planetary Sciences

Research output: Contribution to journal › Article › peer-review

20 Scopus citations

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.

Original language	English (US)
Pages (from-to)	1238-1255
Number of pages	18
Journal	Astrophysical Journal
Volume	724
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/724/2/1238
State	Published - Dec 1 2010

Keywords

Circumstellar matter
Infrared: stars
Planetary systems
Stars: individual (β Leo, o Leo)
Techniques: interferometric

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/724/2/1238

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title = "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.",

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author = "Stock, {Nathan D.} and Su, {Kate Y.L.} and Wilson Liu and Hinz, {Phil M.} and Rieke, {George H.} and Massimo Marengo and Stapelfeldt, {Karl R.} and Hines, {Dean C.} and Trilling, {David E.}",

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AU - Su, Kate Y.L.

AU - Liu, Wilson

AU - Hinz, Phil M.

AU - Rieke, George H.

AU - Marengo, Massimo

AU - Stapelfeldt, Karl R.

AU - Hines, Dean C.

AU - Trilling, David E.

PY - 2010/12/1

Y1 - 2010/12/1

N2 - 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.

AB - 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.

KW - Circumstellar matter

KW - Infrared: stars

KW - Planetary systems

KW - Stars: individual (β Leo, o Leo)

KW - Techniques: interferometric

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The structure of the β leonis debris disk

Abstract

Keywords

ASJC Scopus subject areas

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