Hot Dust in Debris Disks
First Author:
Rachel Akeson
Email: rla AT ipac.caltech.edu
NASA Exoplanet Science Institute, Caltech
770 S. Wilson Ave
Pasadena, CA 91125
Coauthors:
Ciardi, David, NASA Exoplanet Science Institute, Caltech
Millan-Gabet, Rafael, NASA Exoplanet Science Institute, Caltech
Merand, Antoine, European Southern Observatory
di Folco, Emmanuel, Observatoire de Geneve
Monnier, John, University of Michigan
Beichman, Charles, NASA Exoplanet Science Institute, Caltech
Absil, Olivier, LAOG, CNRS and Universite Joseph Fourier
Aufdenberg, Jason, Physical Sciences Department, Embry-Riddle Aeronautical University
McAlister, Hal, Center for High Angular Resolution Astronomy, Georgia State University
ten Brummelaar, Theo, Center for High Angular Resolution Astronomy, Georgia State University
Goldfinger, P.J., Center for High Angular Resolution Astronomy, Georgia State University
Sturmann, Judit, Center for High Angular Resolution Astronomy, Georgia State University
Sturmann, Lazlo, Center for High Angular Resolution Astronomy, Georgia State University
Turner, Nils, Center for High Angular Resolution Astronomy, Georgia State University
Abstract
The size and radial distribution of dust in debris disk systems can be used to infer the location of the large dust-generating bodies and to explore the dynamics of these systems. Near-infrared interferometers provide a unique observational probe of the dust within the central arcsecond and recent high precision observations have revealed excesses at the 1-2% level at 2.2 microns from some early type main sequence stars. These excesses are most consistent with a hot (T>1000 K) dust component very close to the central star. We present new interferometry observations from the Palomar Testbed Interferometer at 1.6 microns to constrain the morphology of the near-infrared excess and discuss the connections between the near and mid-infrared emitting material.
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