Evolution from protoplanetary to debris discs: the transition disc around HD 166191
Article
Article Title | Evolution from protoplanetary to debris discs: the transition disc around HD 166191 |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Kennedy, G. M. (Author), Murphy, S. J. (Author), Lisse, C. M. (Author), Menard, F. (Author), Sitko, M. L. (Author), Wyatt, M. C. (Author), Bayliss, D. D. R. (Author), DeMeo, F. E. (Author), Crawford, K. B. (Author), Kim, D. L. (Author), Rudy, R. J. (Author), Russell, R. W. (Author), Sibthorpe, B. (Author), Skinner, M. A. (Author) and Zhou, G. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 438 (4), pp. 3299-3309 |
Number of Pages | 11 |
Year | 2014 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stt2435 |
Web Address (URL) | https://academic.oup.com/mnras/article/438/4/3299/1101822 |
Abstract | HD 166191 has been identified by several studies as hosting a rare and extremely bright warm debris disc with an additional outer cool disc component. However, an alternative interpretation is that the star hosts a disc that is currently in transition between a full gas disc and a largely gas-free debris disc. With the help of new optical to mid-infrared (IR) spectra and Herschel imaging, we argue that the latter interpretation is supported in several ways: (i) we show that HD 166191 is comoving with the ∼4-Myr-old Herbig Ae star HD 163296, suggesting that the two have the same age; (ii) the disc spectrum of HD 166191 is well matched by a standard radiative transfer model of a gaseous protoplanetary disc with an inner hole and (iii) the HD 166191 mid-IR silicate feature is more consistent with similarly primordial objects. We note some potential issues with the debris disc interpretation that should be considered for such extreme objects, whose lifetime at the current brightness is much shorter than the stellar age, or in the case of the outer component requires a mass comparable to the solid component of the solar nebula. These aspects individually and collectively argue that HD 166191 is a 4-5 Myr old star that hosts a gaseous transition disc. Though it does not argue in favour of either scenario, we find strong evidence for 3-5 μm disc variability. We place HD 166191 in context with discs at different evolutionary stages, showing that it is a potentially important object for understanding the protoplanetary to debris disc transition. |
Keywords | Circumstellar matter; Planets and satellites: formation; Protoplanetary discs; Stars: individual: HD 163296; Stars: individual: HD 166191 |
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 ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | University of Cambridge, United Kingdom |
Heidelberg University, Germany | |
Johns Hopkins University, United States | |
Institute of Planetology and Astrophysics of Grenoble, France | |
University of Cincinnati, United States | |
Australian National University | |
Massachusetts Institute of Technology, United States | |
Aerospace Corporation, United States | |
Netherlands Institute for Space Research, Netherlands | |
Boeing, United States | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q6x49/evolution-from-protoplanetary-to-debris-discs-the-transition-disc-around-hd-166191
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