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Self-gravitating disc candidates around massive young stars
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dc.contributor.author | Forgan, D. H. | |
dc.contributor.author | Ilee, J. D. | |
dc.contributor.author | Cyganowski, C. J. | |
dc.contributor.author | Brogan, C. L. | |
dc.contributor.author | Hunter, T. R. | |
dc.date.accessioned | 2016-10-11T11:30:20Z | |
dc.date.available | 2016-10-11T11:30:20Z | |
dc.date.issued | 2016-11-21 | |
dc.identifier.citation | Forgan , D H , Ilee , J D , Cyganowski , C J , Brogan , C L & Hunter , T R 2016 , ' Self-gravitating disc candidates around massive young stars ' , Monthly Notices of the Royal Astronomical Society , vol. 463 , no. 1 , pp. 957-964 . https://doi.org/10.1093/mnras/stw1917 | en |
dc.identifier.issn | 1365-2966 | |
dc.identifier.other | PURE: 246547238 | |
dc.identifier.other | PURE UUID: 203d002b-8c1a-474c-b1ff-445df4287dc8 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1608.05539v1 | |
dc.identifier.other | WOS: 000386464900076 | |
dc.identifier.other | Scopus: 85014357866 | |
dc.identifier.uri | https://hdl.handle.net/10023/9642 | |
dc.description | DHF gratefully acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG. JDI gratefully acknowledges support from the DISCSIM project, grant agreement 341137, funded by the European Research Council under ERC-2013-ADG. CJC acknowledges support from STFC grant ST/M001296/1. | en |
dc.description.abstract | There have been several recent detections of candidate Keplerian discs around massive young protostars. Given the relatively large disc-to-star mass ratios in these systems, and their young ages, it is worth investigating their propensity to becoming self-gravitating. To this end, we compute self-consistent, semi-analytic models of putative self-gravitating discs for five candidate disc systems. Our aim is not to fit exactly the observations, but to demonstrate that the expected dust continuum emission from marginally unstable self-gravitating discs can be quite weak, due to high optical depth at the mid-plane even at millimetre wavelengths. In the best cases, the models produce ‘observable’ disc masses within a factor of <1.5 of those observed, with mid-plane dust temperatures comparable to measured temperatures from molecular line emission. We find in two cases that a self-gravitating disc model compares well with observations. If these discs are self-gravitating, they satisfy the conditions for disc fragmentation in their outer regions. These systems may hence have as-yet-unresolved low-mass stellar companions, and are thus promising targets for future high angular resolution observations. | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.rights | © 2016, the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at mnras.oxfordjournals.org / https://doi.org/10.1093/mnras/stw1917 | en |
dc.subject | Stars: formation | en |
dc.subject | Stars: massive | en |
dc.subject | Stars: pre-main sequence | en |
dc.subject | Stars: protostars | en |
dc.subject | Radio continuum: stars | en |
dc.subject | Submillimetre: stars | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | T-NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Self-gravitating disc candidates around massive young stars | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.description.version | Postprint | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/stw1917 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/M001296/1 | en |
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