The Twofold Debris Disk Around HD113766 A Warm And Cold Dust As Seen With VLTI/MIDI And Herschel/PACS

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dc.contributor.utaustinauthorOliveira, I.en_US
dc.creatorOlofsson, J.en_US
dc.creatorHenning, T.en_US
dc.creatorNielbock, M.en_US
dc.creatorAugereau, J. C.en_US
dc.creatorJuhasz, A.en_US
dc.creatorOliveira, I.en_US
dc.creatorAbsil, O.en_US
dc.creatorTamanai, A.en_US
dc.date.accessioned2016-04-22T19:48:22Z
dc.date.available2016-04-22T19:48:22Z
dc.date.issued2013-03en
dc.description.abstractContext. Warm debris disks are a sub-sample of the large population of debris disks, and display excess emission in the mid-infrared. Around solar-type stars, very few objects (similar to 2% of all debris disks) show emission features in mid-IR spectroscopic observations that are attributed to small, warm silicate dust grains. The origin of this warm dust could be explained either by a recent catastrophic collision between several bodies or by transport from an outer belt similar to the Kuiper belt in the solar system. Aims. We present and analyze new far-IR Herschel/PACS photometric observations, supplemented by new and archival ground-based data in the mid-IR (VLTI/MIDI and VLT/VISIR), for one of these rare systems: the 10-16 Myr old debris disk around HD 113766 A. We improve an existing model to account for these new observations. Methods. We implemented the contribution of an outer planetesimal belt in the DEBRA code, and successfully used it to model the spectral energy distribution (SED) as well as complementary observations, notably MIDI data. We better constrain the spatial distribution of the dust and its composition. Results. We underline the limitations of SED modeling and the need for spatially resolved observations. We improve existing models and increase our understanding of the disk around HD 113766 A. We find that the system is best described by an inner disk located within the first AU, well constrained by the MIDI data, and an outer disk located between 9-13 AU. In the inner dust belt, our previous finding of Fe-rich crystalline olivine grains still holds. We do not observe time variability of the emission features over at least an eight-year time span in an environment subjected to strong radiation pressure. Conclusions. The time stability of the emission features indicates that mu m-sized dust grains are constantly replenished from the same reservoir, with a possible depletion of sub-mu m-sized grains. We suggest that the emission features may arise from multi-composition aggregates. We discuss possible scenarios concerning the origin of the warm dust observed around HD 113766 A. The compactness of the innermost regions as probed by the MIDI visibilities and the dust composition suggest that we are witnessing the results of (at least) one collision between partially differentiated bodies, in an environment possibly rendered unstable by terrestrial planetary formation.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipFrench National Research Agency (ANR) ANR-2010 BLAN-0505-01en_US
dc.identifierdoi:10.15781/T24V32
dc.identifier.citationOlofsson, Johan, Th Henning, Markus Nielbock, J-C. Augereau, Attila Juhasz, Isa Oliveira, Olivier Absil, and Akemi Tamanai. >The twofold debris disk around HD 113766 a-warm and cold dust as seen with VLTI/Midi and herschel/pacs.> Astronomy & Astrophysics, Vol. 551 (Mar., 2013): A134.en_US
dc.identifier.doi10.1051/0004-6361/201220904en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/2152/34539
dc.language.isoEnglishen_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectstars: individual: hd 113766 aen_US
dc.subjectzodiacal dusten_US
dc.subjectcircumstellar matteren_US
dc.subjectinfrared: starsen_US
dc.subjecttechniques: spectroscopicen_US
dc.subjecttechniques: high angularen_US
dc.subjectresolutionen_US
dc.subjectinterstellar silicate mineralogyen_US
dc.subjectterrestrial planet formationen_US
dc.subjectsolar-type starsen_US
dc.subjectkuiper-belten_US
dc.subjectspitzer mipsen_US
dc.subjecthd 172555en_US
dc.subjecthot dusten_US
dc.subjecttau-cetien_US
dc.subjectt-taurien_US
dc.subjectgrainsen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Twofold Debris Disk Around HD113766 A Warm And Cold Dust As Seen With VLTI/MIDI And Herschel/PACSen_US
dc.typeArticleen_US

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