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Modelling the Huge, Herschel-Resolved Debris Ring around HD 207129
External Online Source: doi:10.1051/0004-6361/201117731
Author and Affiliation:
Lohne, T.(Friedrich-Schiller Univ., Astrophysikalisches Inst. und Universitatssternwarte, Jena, Germany);
Augereau, J. C.(Centre National de la Recherche Scientifique, Grenoble, France);
Ertel, S.(Kiel Univ., Institut fur Theoretische Physik und Astrophysik, Germany);
Marshall, J. P.(Universidad Autonoma de Madrid, Cantoblanco, Spain);
Mora, A.(Villanueva de la Canada, Madrid, Spain);
Absil, O.(Liege Univ., Belgium);
Stapelfeldt, K.(Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, United States);
Thebault, P.(Observatoire de Paris, France);
Bayo, A.(European Southern Observatory, Santiago, Chile);
del Burgo, C.(UNINOVA, Caparica, Portugal);
Danchi, W.(NASA Goddard Space Flight Center, Greenbelt, MD, United States);
Krivov, A. V.(Friedrich-Schiller Univ., Astrophysikalisches Inst. und Universitatssternwarte, Jena, Germany);
Lebreton, J.(Centre National de la Recherche Scientifique, Grenoble, France);
Letawe, G.(Liege Univ., Belgium);
Magain, P.(Liege Univ., Belgium);
Maldonado, J.(Universidad Autonoma de Madrid, Cantoblanco, Spain);
Montesinos, B.(Centro de Astrobiologia, Madrid, Spain);
Pilbratt, G. L.(European Space Research and Technology Centre, Noordwijk, Netherlands);
White, G. J.(Open Univ., Milton Keynes, United Kingdom);
Wolf, S.(Kiel Univ., Institut fur Theoretische Physik und Astrophysik, Germany)
Abstract: Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks. and probably planetesimals, arc common features of stellar systems. As the mechanisms of their fonnation and evolution are linked to those of planetary bodies, they provide valuable infonnation. 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(sup -2) Earth masses in dust, with typical grain sizes in the planetesimal beh ranging from 4 to 7 micrometers. 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 micrometers. 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.
Publication Date: Nov 09, 2011
Document ID:
20120015727
(Acquired Nov 16, 2012)
Subject Category: ASTRONOMY
Report/Patent Number: GSFC.JA.7087.2012
Document Type: Journal Article
Publication Information: Astronomy and Astrophysics; Volume 537; A110
Publisher Information: European Southern Observatory, Munich,, Germany
Contract/Grant/Task Num: DFG Lo 1715/1-1; DFG Kr 2164/9-1; DFG Wo 857/7-1; AYA 2008-01727; PEst-OE/EEI/UI0066/2011
Financial Sponsor: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Organization Source: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Description: 15p; In English; Original contains color and black and white illustrations
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: ASYMMETRY; CHEMICAL COMPOSITION; COSMIC DUST; IMAGING TECHNIQUES; INTERPLANETARY MEDIUM; LIGHT SCATTERING; MATHEMATICAL MODELS; OBSERVATORIES; PRE-MAIN SEQUENCE STARS; RADIAL DISTRIBUTION; SPACE DEBRIS; SPECTRAL ENERGY DISTRIBUTION; STARS
Availability Source: Other Sources
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