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The debris disk – terrestrial planet connection

Published online by Cambridge University Press:  10 November 2011

Sean N. Raymond ,
Philip J. Armitage ,
Amaya Moro-Martín ,
Mark Booth ,
Mark C. Wyatt ,
John C. Armstrong ,
Avi M. Mandell  and
Franck Selsis
Sean N. Raymond
Affiliation:
Université de Bordeaux, Observatoire Aquitain des Sciences de l'Univers, 2 rue de l'Observatoire, BP 89, F-33271 Floirac Cedex, France email: [email protected] CNRS, UMR 5804, Laboratoire d'Astrophysique de Bordeaux, 2 rue de l'Observatoire, BP 89, F-33271 Floirac Cedex, France
Philip J. Armitage
Affiliation:
JILA, University of Colorado, Boulder CO 80309, USA Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309, USA
Amaya Moro-Martín
Affiliation:
Departamento de Astrofisica, CAB (CSIC-INTA), Instituto Nacional de Tecnica Aeroespacial, Torrejon de Ardoz, 28850, Madrid, Spain Department of Astrophysical Sciences, Princeton University, Peyton Hall, Ivy Lane, Princeton, NJ 08544, USA
Mark Booth
Affiliation:
Institute of Astronomy, Cambridge University, Madingley Road, Cambridge, UK
Mark C. Wyatt
Affiliation:
Institute of Astronomy, Cambridge University, Madingley Road, Cambridge, UK
John C. Armstrong
Affiliation:
Department of Physics, Weber State University, Ogden, UT, USA
Avi M. Mandell
Affiliation:
NASA Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
Franck Selsis
Affiliation:
Université de Bordeaux, Observatoire Aquitain des Sciences de l'Univers, 2 rue de l'Observatoire, BP 89, F-33271 Floirac Cedex, France email: [email protected] CNRS, UMR 5804, Laboratoire d'Astrophysique de Bordeaux, 2 rue de l'Observatoire, BP 89, F-33271 Floirac Cedex, France
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Abstract

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The eccentric orbits of the known extrasolar giant planets provide evidence that most planet-forming environments undergo violent dynamical instabilities. Here, we numerically simulate the impact of giant planet instabilities on planetary systems as a whole. We find that populations of inner rocky and outer icy bodies are both shaped by the giant planet dynamics and are naturally correlated. Strong instabilities – those with very eccentric surviving giant planets – completely clear out their inner and outer regions. In contrast, systems with stable or low-mass giant planets form terrestrial planets in their inner regions and outer icy bodies produce dust that is observable as debris disks at mid-infrared wavelengths. Fifteen to twenty percent of old stars are observed to have bright debris disks (at λ ~ 70μm) and we predict that these signpost dynamically calm environments that should contain terrestrial planets.

Keywords

planetary systems: formationdebris disksmethods: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 82 - 88
Copyright
Copyright © International Astronomical Union 2011

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