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dc.contributor.authorHall, Cassandra
dc.contributor.authorForgan, Duncan
dc.contributor.authorRice, Ken
dc.contributor.authorHarries, Tim J.
dc.contributor.authorKlaassen, Pamela D.
dc.contributor.authorBiller, Beth
dc.date.accessioned2016-05-05T14:32:57Z
dc.date.available2016-05-05T14:32:57Z
dc.date.issued2016-05-01
dc.identifier.citationHall , C , Forgan , D , Rice , K , Harries , T J , Klaassen , P D & Biller , B 2016 , ' Directly observing continuum emission from self-gravitating spiral waves ' , Monthly Notices of the Royal Astronomical Society , vol. 458 , no. 1 , pp. 306-318 . https://doi.org/10.1093/mnras/stw296en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 242359924
dc.identifier.otherPURE UUID: 432230e3-058b-4220-897d-ad7479e244c2
dc.identifier.otherRIS: urn:69467705939DFC57FC4A9957F92CBA88
dc.identifier.otherScopus: 84963729917
dc.identifier.otherWOS: 000374568900018
dc.identifier.urihttp://hdl.handle.net/10023/8729
dc.descriptionKR and BB gratefully acknowledge support from STFC grant ST/M001229/1. DF gratefully acknowledges support from the ECOGAL ERC advanced grant. Some calculations for this paper were performed on the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital fund of BIS, and the University of Exeter, and on the Complexity DiRAC Facility jointly funded by STFC and the Large Facilities Capital Fund of BIS. TJH acknowledges funding from Exeter’s STFC Consolidated Grant (ST/J001627/1).en
dc.description.abstractWe use a simple, self-consistent, self-gravitating semi-analytic disc model to conduct an examination of the parameter space in which self-gravitating discs may exist. We then use Monte Carlo radiative transfer to generate synthetic Atacama Large Millimeter/submillimeter Array (ALMA) images of these self-gravitating discs to determine the subset of this parameter space in which they generate non-axisymmetric structure that is potentially detectable by ALMA. Recently, several transition discs have been observed to have non-axisymmetric structure that extends out to large radii. It has been suggested that one possible origin of these asymmetries could be spiral density waves induced by disc self-gravity. We use our simple model to see if these discs exist in the region of parameter space where self-gravity could feasibly explain these spiral features. We find that for self-gravity to play a role in these systems typically requires a disc mass around an order of magnitude higher than the observed disc masses for the systems. The spiral amplitudes produced by self-gravity in the local approximation are relatively weak when compared to amplitudes produced by tidal interactions, or spirals launched at Lindblad resonances due to embedded planets in the disc. As such, we ultimately caution against diagnosing spiral features as being due to self-gravity, unless the disc exists in the very narrow region of parameter space where the spiral wave amplitudes are large enough to produce detectable features, but not so large as to cause the disc to fragment.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stw296en
dc.subjectRadiative transferen
dc.subjectPlanets and satellites: formationen
dc.subjectProtoplanetary discsen
dc.subjectStarts: pre-main-sequenceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleDirectly observing continuum emission from self-gravitating spiral wavesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw296
dc.description.statusPeer revieweden


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