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dc.contributor.authorGledhill, T.
dc.contributor.authorYates, J.A.
dc.identifier.citationGledhill , T & Yates , J A 2003 , ' Mid-infrared imaging of the dust shell around the post-asymptotic giant branch star HD 161796 ' , Monthly Notices of the Royal Astronomical Society , vol. 343 , no. 3 , pp. 880-890 .
dc.identifier.otherPURE: 175748
dc.identifier.otherPURE UUID: dbe634ed-23c9-4b70-b6de-791e48613c80
dc.identifier.otherdspace: 2299/4273
dc.identifier.otherScopus: 0142055126
dc.identifier.otherORCID: /0000-0002-2859-4600/work/30779781
dc.description‘The definitive version is available at '. Copyright Blackwell Publishing. DOI: 10.1046/j.1365-8711.2003.06732.x [Full text of this article is not available in the UHRA]
dc.description.abstractWe present mid-infrared (IR) images of HD 161796 (IRAS 17436+5003), taken with the OSCIR imager on the Gemini North Telescope, that resolve for the first time the thermal emission structure of the dust shell around this post-asymptotic giant branch (AGB) star. As well as a basic axisymmetric structure, the observations show deviations from axisymmetry in the dust density and a twist in the symmetry axis. Modelling of the mid-IR images and of the spectral energy distribution from ultraviolet to submillimetre wavelengths reproduces all of the axisymmetric features with an equator-to-pole density contrast of 6: 1 and an inclination of the symmetry axis of 10° to the plane of the sky. We find that a model incorporating small (0.01μm) grains and a steep (∝a−6) power-law size distribution can successfully account for the thermal emission and for the observed degrees of near-IR polarization. Assuming a distance of 1.2 kpc to HD 161796, the stellar luminosity is 3.4 × 103 L⊙ and the mass of the shell is ∼0.7 M⊙ . This is consistent with a star of initial mass between 1 and 2 M⊙ that has undergone an intensive (2.2 × 10−4 M⊙ yr−1) phase of mass loss lasting about 3000 yr at the end of the AGB. A current stellar mass of 0.56 M⊙ , as indicated by the luminosity, suggests that HD 161796 is a few hundred years into its post-AGB evolution and will take about 5000 yr to evolve from its present temperature of 7500 K to become the central star of an extended elliptical planetary nebula.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleMid-infrared imaging of the dust shell around the post-asymptotic giant branch star HD 161796en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

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