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Determining the Origin of Inner Planetary System Debris Orbiting the Dustiest Main Sequence Stars

Published online by Cambridge University Press:  29 April 2014

Carl Melis ,
B. Zuckerman ,
Joseph H. Rhee ,
Inseok Song ,
S. J. Murphy  and
M. S. Bessell
Carl Melis
Affiliation:
Center for Astrophysics and Space Sciences, University of California, San Diego, California 92093-0424, USA; email: cmelis@ucsd.edu
B. Zuckerman
Affiliation:
Department of Physics and Astronomy, University of California, Los Angeles, California 90095-1547, USA
Joseph H. Rhee
Affiliation:
Department of Physics and Astronomy, California State Polytechnic University, Pomona, Pomona, California 91768, USA
Inseok Song
Affiliation:
Department of Physics and Astronomy, University of Georgia, Athens, Georgia 30602, USA
S. J. Murphy
Affiliation:
Research School of Astronomy and Astrophysics, College of Mathematical and Physical Sciences, The Australian National University, Cotter Road, Weston Creek, Australian Capital Territory 2611, Australia
M. S. Bessell
Affiliation:
Research School of Astronomy and Astrophysics, College of Mathematical and Physical Sciences, The Australian National University, Cotter Road, Weston Creek, Australian Capital Territory 2611, Australia
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Abstract

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We develop a means to distinguish between warm dusty circumstellar debris disks produced by steady state collisional evolution of a planetesimal belt or through transient events.

Keywords

planets and satellites: formationcircumstellar matterplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 273 - 277
Copyright
Copyright © International Astronomical Union 2014 

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