Multi-wavelength modeling of the spatially resolved debris disk of HD 107146
Institut für Theoretische Physik und Astrophysik,
Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24098
2 Department of Physics and Astronomy, State University of New York, Stony Brook, NY 11794-3800, USA
3 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
4 Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
5 Institute for Astronomy, ETH Zürich, Wolfgang-Pauli-Straße 27, 8093 Zürich, Switzerland
6 Department of Physics & Astronomy, University of Alabama, 326 Gallalee, Tuscaloosa, AL 35487-0324, USA
Accepted: 1 July 2011
Aims. We aim to constrain the location, composition, and dynamical state of planetesimal populations and dust around the young, sun-like (G2 V) star HD 107146.
Methods. We consider coronagraphic observations obtained with the Advanced Camera for Surveys (HST/ACS) onboard the Hubble Space Telescope (HST) in broad V (λc ≈ 0.6 μm) and broad I (λc ≈ 0.8 μm) filters, a resolved 1.3 mm map obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA), Spitzer/IRS low resolution spectra in the range of 7.6 μm to 37.0 μm, and the spectral energy distribution (SED) of the object at wavelengths ranging from 3.5 μm to 3.1 mm. We complement these data with new coronagraphic high resolution observations of the debris disk using the Near Infrared Camera and Multi-Object Spectrometer (HST/NICMOS) aboard the HST in the F110W filter (λc ≈ 1.1 μm). The SED and images of the disk in scattered light as well as in thermal reemission are combined in our modeling using a parameterized model for the disk density distribution and optical properties of the dust.
Results. A detailed analytical model of the debris disk around HD 107146 is presented that allows us to reproduce the almost entire set of spatially resolved and unresolved multi-wavelength observations. Considering the variety of complementary observational data, we are able to break the degeneracies produced by modeling SED data alone. We find the disk to be an extended ring with a peak surface density at 131 AU. Furthermore, we find evidence for an additional, inner disk probably composed of small grains released at the inner edge of the outer disk and moving inwards due to Poynting-Robertson drag. A birth ring scenario (i.e., a more or less broad ring of planetesimals creating the dust disk trough collisions) is found to be the most likely explanation of the ringlike shape of the disk.
Key words: stars: individual: HD 107146 / techniques: high angular resolution / methods: data analysis / circumstellar matter / infrared: stars
© ESO, 2011