Multi-wavelength, spatially resolved modelling of HD 48682's debris disc
Article
Article Title | Multi-wavelength, spatially resolved modelling of HD 48682's debris disc |
---|---|
ERA Journal ID | 1074 |
Article Category | Article |
Authors | Hengst, S. (Author), Marshall, J. P. (Author), Horner, J. (Author) and Marsden, S. C. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 497 (1), pp. 1098-1109 |
Number of Pages | 12 |
Year | 2020 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/staa1972 |
Web Address (URL) | https://academic.oup.com/mnras/article/497/1/1098/5868829 |
Abstract | Asteroids and comets (planetesimals) are created in gas- and dust-rich protoplanetary discs. The presence of these planetesimals around main-sequence stars is usually inferred from the detection of excess continuum emission at infrared wavelengths from dust grains produced by destructive processes within these discs. Modelling of the disc structure and dust grain properties for those discs is often hindered by the absence of any meaningful constraint on the location and spatial extent of the disc. Multi-wavelength, spatially resolved imaging is thus invaluable in refining the interpretation of these systems. Observations of HD 48682 at far-infrared (Spitzer, Herschel) and sub-millimetre (JCMT, SMA) wavelengths indicated the presence of an extended, cold debris disc with a blackbody temperature of 57.9 ± 0.7 K. Here, we combined these data to perform a comprehensive study of the disc architecture and its implications for the dust grain properties. The deconvolved images revealed a cold debris belt, verified by combining a 3D radiative transfer dust continuum model with image analysis to replicate the structure using a single, axisymmetric annulus. A Markov chain Monte Carlo analysis calculated the maximum likelihood of HD48682's disc radius ( $R_{\rm disc} = 89^{+17}_{-20}~$ au), fractional width ( $\Delta R_{\rm disc} = 0.41^{+0.27}_{-0.20}$ ), position angle ( $\theta = 66{_{.}^{\circ}} 3^{+4.5}_{-4.9}$ ), and inclination ( $\phi = 112{_{.}^{\circ}} 5^{+4.2}_{-4.2}$ ). HD 48682 has been revealed to host a collisionally active, broad disc whose emission is dominated by small dust grains, s<SUB>min</SUB> ∼ 0.6 μm, and a size distribution exponent of 3.60 ± 0.02. A correction has been published: Monthly Notices of the Royal Astronomical Society, Volume 499, Issue 1, November 2020, Pages 616–617, https://doi.org/10.1093/mnras/staa2874 |
Keywords | circumstellar matter; stars: individual: HD 48682; infrared:; planetary systems; infrared: stars; Astrophysics - Earth and Planetary; Astrophysics; Astrophysics - Astrophysics of Galaxies; Astrophysics -; Solar and Stellar Astrophysics |
Related Output | |
Is reviewed by | Erratum: Multi-wavelength, spatially resolved modelling of HD 48682’s debris disc |
Is part of | Dust Grain Dynamics in Debris Discs |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Centre for Astrophysics |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q5yx3/multi-wavelength-spatially-resolved-modelling-of-hd-48682-s-debris-disc
Download files
170
total views120
total downloads6
views this month1
downloads this month