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dc.contributor.authorScholz, Aleks
dc.contributor.authorNatta, Antonella
dc.contributor.authorBozhinova, Inna
dc.contributor.authorPetkova, Maya
dc.contributor.authorRelles, Howard
dc.contributor.authorEislöffel, Jochen
dc.date.accessioned2019-02-20T15:30:05Z
dc.date.available2019-02-20T15:30:05Z
dc.date.issued2019-04-11
dc.identifier.citationScholz , A , Natta , A , Bozhinova , I , Petkova , M , Relles , H & Eislöffel , J 2019 , ' Clumpy dust rings around non-accreting young stars ' , Monthly Notices of the Royal Astronomical Society , vol. 484 , no. 3 , pp. 4260–4272 . https://doi.org/10.1093/mnras/stz269en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 257807773
dc.identifier.otherPURE UUID: dff2f8bf-cd51-46d7-9e09-c86b0d11f344
dc.identifier.otherBibCode: 2019MNRAS.tmp..265S
dc.identifier.otherBibCode: 2019MNRAS.484.4260S
dc.identifier.otherScopus: 85067106947
dc.identifier.otherWOS: 000462410300101
dc.identifier.urihttp://hdl.handle.net/10023/17103
dc.descriptionThis project was supported by STFC grant ST/R000824/1 to AS. MP acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907), and from the ERC under ERC-2011-ADG via the ECOGAL project (grant agreement number 291227).en
dc.description.abstractWe investigate four young, but non-accreting, very low mass stars in Orion, which show irregular eclipses by circumstellar dust. The eclipses are not recurring periodically, are variable in depth, lack a flat bottom, and their duration is comparable to the typical time-scale between eclipses. The dimming is associated with reddening consistent with dust extinction. Taken together this implies the presence of rings around these four stars, with radii ranging from 0.01 to 40 au, comprised of optically thin dust clouds. The stars also show infrared excess indicating the presence of evolved circumstellar discs, with orders of magnitude more material than needed for the eclipses. However, the rings need to cover an opening angle of about 20 deg to explain how common these variable stars are in the coeval population in the same region, which is more extended than a typical disc. Thus, we propose that the rings may not be part of the discs, but instead separate structures with larger scale heights. To be sustained over years, the rings need to be replenished by dust from the disc or gravitationally bound to an object (e.g. planets or planetesimals). These four stars belong to a growing and diverse class of post-T Tauri stars with dips or eclipses in their light curves. Dusty rings with scale heights exceeding those of discs may be a common phenomenon at stellar ages between 5 and 10 Myr, in the transition from accretion discs to debris discs. These structures could be caused by migrating planets and may be signposts for the presence of young planetary systems.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2019, the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been 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://doi.org/10.1093/mnras/stz269en
dc.subjectOccultationsen
dc.subjectPlanets and satellites: formationen
dc.subjectProtoplanetary discsen
dc.subjectCircumstellar matteren
dc.subjectStars: pre-main-sequenceen
dc.subjectDusten
dc.subjectExtinctionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleClumpy dust rings around non-accreting young starsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz269
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019MNRAS.tmp..265Sen
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019MNRAS.484.4260Sen


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