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Title:
The Debris Disk Around HR 8799
Authors:
Su, K. Y. L.; Rieke, G. H.; Stapelfeldt, K. R.; Malhotra, R.; Bryden, G.; Smith, P. S.; Misselt, K. A.; Moro-Martin, A.; Williams, J. P.
Affiliation:
AA(Steward Observatory, University of Arizona, 933 N Cherry Avenue, Tucson, AZ 85721, USA ), AB(Steward Observatory, University of Arizona, 933 N Cherry Avenue, Tucson, AZ 85721, USA ), AC(JPL/Caltech, 4800 Oak Grove Drive, Pasadena, CA 91109, USA ), AD(Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA ), AE(JPL/Caltech, 4800 Oak Grove Drive, Pasadena, CA 91109, USA ), AF(Steward Observatory, University of Arizona, 933 N Cherry Avenue, Tucson, AZ 85721, USA ), AG(Steward Observatory, University of Arizona, 933 N Cherry Avenue, Tucson, AZ 85721, USA ), AH(Department of Astrophysical Science, Princeton University, Princeton, NJ 08544, USA ; Center for Astrobiology (CSIC-INTA), Madrid, Spain ), AI(Institute for Astronomy, University of Hawaii, USA)
Publication:
The Astrophysical Journal, Volume 705, Issue 1, pp. 314-327 (2009). (ApJ Homepage)
Publication Date:
11/2009
Origin:
IOP
ApJ Keywords:
circumstellar matter, infrared: stars, planetary systems, stars: individual: HR 8799
DOI:
10.1088/0004-637X/705/1/314
Bibliographic Code:
2009ApJ...705..314S

Abstract

We have obtained a full suite of Spitzer observations to characterize the debris disk around HR 8799 and to explore how its properties are related to the recently discovered set of three massive planets orbiting the star. We distinguish three components to the debris system: (1) warm dust (T ~ 150 K) orbiting within the innermost planet; (2) a broad zone of cold dust (T ~ 45 K) with a sharp inner edge orbiting just outside the outermost planet and presumably sculpted by it; and (3) a dramatic halo of small grains originating in the cold dust component. The high level of dynamical activity implied by this halo may arise due to enhanced gravitational stirring by the massive planets. The relatively young age of HR 8799 places it in an important early stage of development and may provide some help in understanding the interaction of planets and planetary debris, an important process in the evolution of our own solar system.
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