Multi-wavelength modeling of the spatially resolved debris disk of HD107146

Show simple item record Ertel, S. Wolf, S. Metchev, S. Schneider, G. Carpenter, J. M. Meyer, M. R. Hillenbrand, L. A. Silverstone, M. D.
dc.contributor.other University of Kiel
dc.contributor.other State University of New York (SUNY) System
dc.contributor.other State University of New York (SUNY) Stony Brook
dc.contributor.other University of Arizona
dc.contributor.other California Institute of Technology
dc.contributor.other Swiss Federal Institutes of Technology Domain
dc.contributor.other ETH Zurich
dc.contributor.other University of Alabama Tuscaloosa 2019-06-17T19:19:48Z 2019-06-17T19:19:48Z 2011 2001-09-15
dc.identifier.citation Ertel, S., et al. (2011): Multi-Wavelength Modeling of the Spatially Resolved Debris Disk of HD 107146. Astronomy and Astrophysics, 525(A132). DOI:
dc.description.abstract Aims. We aim to constrain the location, composition, and dynamical state of planetesimal populations and dust around the young, sun-like (G2V) star HD107146. Methods. We consider coronagraphic observations obtained with the Advanced Camera for Surveys (HST/ACS) onboard the Hubble Space Telescope (HST) in broad V (lambda(c) approximate to 0.6 mu m) and broad I (lambda(c) approximate to 0.8 mu m) 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 mu m to 37.0 mu m, and the spectral energy distribution (SED) of the object at wavelengths ranging from 3.5 mu m 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 (lambda(c) approximate to 1.1 mu m). 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 HD107146 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. en_US
dc.format.mimetype application/pdf
dc.language English
dc.language.iso en_US
dc.publisher EDP Sciences
dc.subject stars: individual: HD 107146
dc.subject techniques: high angular resolution
dc.subject methods: data analysis
dc.subject circumstellar matter
dc.subject infrared: stars
dc.subject SUN-LIKE STARS
dc.subject GRAIN-SIZE
dc.subject BETA-PICTORIS
dc.subject DUST
dc.subject EVOLUTION
dc.subject Astronomy & Astrophysics
dc.title Multi-wavelength modeling of the spatially resolved debris disk of HD107146 en_US
dc.type text
dc.type Article
dc.rights.holder ESO
dc.identifier.doi 10.1051/0004-6361/201015910

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