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

dc.contributor.authorErtel, S.
dc.contributor.authorWolf, S.
dc.contributor.authorMetchev, S.
dc.contributor.authorSchneider, G.
dc.contributor.authorCarpenter, J. M.
dc.contributor.authorMeyer, M. R.
dc.contributor.authorHillenbrand, L. A.
dc.contributor.authorSilverstone, M. D.
dc.contributor.otherUniversity of Kiel
dc.contributor.otherState University of New York (SUNY) System
dc.contributor.otherState University of New York (SUNY) Stony Brook
dc.contributor.otherUniversity of Arizona
dc.contributor.otherCalifornia Institute of Technology
dc.contributor.otherSwiss Federal Institutes of Technology Domain
dc.contributor.otherETH Zurich
dc.contributor.otherUniversity of Alabama Tuscaloosa
dc.date.accessioned2019-06-17T19:19:48Z
dc.date.available2019-06-17T19:19:48Z
dc.date.copyright2011
dc.date.issued2001-09-15
dc.description.abstractAims. 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.mimetypeapplication/pdf
dc.identifier.citationErtel, S., et al. (2011): Multi-Wavelength Modeling of the Spatially Resolved Debris Disk of HD 107146. Astronomy and Astrophysics, 525(A132). DOI: https://doi.org/10.1051/0004-6361/201015910
dc.identifier.doi10.1051/0004-6361/201015910
dc.identifier.orcidhttps://orcid.org/0000-0001-7841-3452
dc.identifier.orcidhttps://orcid.org/0000-0003-3050-8203
dc.identifier.orcidhttps://orcid.org/0000-0003-2251-0602
dc.identifier.urihttp://ir.ua.edu/handle/123456789/5772
dc.languageEnglish
dc.language.isoen_US
dc.publisherEDP Sciences
dc.rights.holderESO
dc.subjectstars: individual: HD 107146
dc.subjecttechniques: high angular resolution
dc.subjectmethods: data analysis
dc.subjectcircumstellar matter
dc.subjectinfrared: stars
dc.subjectMAIN-SEQUENCE STARS
dc.subjectSUN-LIKE STARS
dc.subjectPLANETARY SYSTEMS
dc.subjectGRAIN-SIZE
dc.subjectCIRCUMSTELLAR DISK
dc.subjectBETA-PICTORIS
dc.subjectDUST
dc.subjectEVOLUTION
dc.subjectSUBMILLIMETER
dc.subjectDISTRIBUTIONS
dc.subjectAstronomy & Astrophysics
dc.titleMulti-wavelength modeling of the spatially resolved debris disk of HD107146en_US
dc.typetext
dc.typeArticle
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