Volume 537, January 2012
|Number of page(s)||15|
|Section||Interstellar and circumstellar matter|
|Published online||17 January 2012|
Modelling the huge, Herschel-resolved debris ring around HD 207129⋆
1 Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany
2 UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France
3 Christian-Albrechts-Universität zu Kiel, Institut für Theoretische Physik und Astrophysik, Leibnizstr. 15, 24098 Kiel, Germany
4 Departmento Física Teórica, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
5 ESA-ESAC Gaia SOC. PO Box 78, 28691, Villanueva de la Cañada Madrid, Spain
6 Institut d’Astrophysique et de Géophysique, Université de Liège, allée du 6 août 17, 4000 Liège, Belgium
7 Departmento de Astrofísica, Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
8 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
9 LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France
10 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
11 UNINOVA-CA3, Campus da Caparica, Quinta da Torre, Monte de Caparica, 2825-149 Caparica, Portugal
12 ESA Astrophysics & Fundamental Physics Missions Division, ESTEC/SRE-SA, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
13 Department of Physics and Astrophysics, Open University, Walton Hall, Milton Keynes MK7 6AA, UK
14 Rutherford Appleton Laboratory, Chilton OX11 0QX, UK
15 NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics, Code 667, Greenbelt, MD 20771, USA
Received: 19 July 2011
Accepted: 9 November 2011
Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modelling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution and Herschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10-2 Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7 μm. We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70 μm. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170–190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk.
Key words: interplanetary medium / stars: individual: HD 207129
© ESO, 2012
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