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dc.contributor.authorSicilia-Aguilar, A.
dc.contributor.authorBanzatti, A.
dc.contributor.authorCarmona, A.
dc.contributor.authorStolker, T.
dc.contributor.authorKama, M.
dc.contributor.authorMendigutía, I
dc.contributor.authorGarufi, A.
dc.contributor.authorFlaherty, K.
dc.contributor.authorMarel, N. van der
dc.contributor.authorGreaves, J.
dc.date.accessioned2017-06-13T23:35:57Z
dc.date.available2017-06-13T23:35:57Z
dc.date.issued2016-12-13
dc.identifier.citationSicilia-Aguilar , A , Banzatti , A , Carmona , A , Stolker , T , Kama , M , Mendigutía , I , Garufi , A , Flaherty , K , Marel , N V D & Greaves , J 2016 , ' A 'Rosetta Stone' for protoplanetary disks : the synergy of multi-wavelength observations ' , Publications of the Astronomical Society of Australia , vol. 33 , e059 . https://doi.org/10.1017/pasa.2016.56en
dc.identifier.issn1323-3580
dc.identifier.otherPURE: 247488979
dc.identifier.otherPURE UUID: 19bef956-1793-4a4e-9764-f9a4581ca719
dc.identifier.otherArXiv: http://arxiv.org/abs/1611.01798v1
dc.identifier.otherScopus: 85004011314
dc.identifier.otherWOS: 000390808600001
dc.identifier.urihttp://hdl.handle.net/10023/10988
dc.description.abstractThe recent progress in instrumentation and telescope development has brought us different ways to observe protoplanetary disks, including interferometers, space missions, adaptive optics, polarimetry, and time- and spectrally-resolved data. While the new facilities have changed the way we can tackle the existing open problems in disk structure and evolution, there is a substantial lack of interconnection between different observing techniques and their user communities. Here, we explore the complementarity of some of the state-of-the-art observing techniques, and how they can be brought together in a collective effort to understand how disks evolve and disperse at the time of planet formation. This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh, 2016. Its goal is to clarify where multi-wavelength observations of disks converge in unveiling disk structure and evolution, and where they diverge and challenge our current understanding. We discuss caveats that should be considered when linking results from different observations, or when drawing conclusions based on limited datasets (in terms of wavelength or sample). We focus on disk properties that are currently being revolutionized by multi-wavelength observations. Specifically: the inner disk radius, holes and gaps and their link to large-scale disk structures, the disk mass, and the accretion rate. We discuss how the links between them, as well as the apparent contradictions, can help us to disentangle the disk physics and to learn about disk evolution.
dc.format.extent31
dc.language.isoeng
dc.relation.ispartofPublications of the Astronomical Society of Australiaen
dc.rights© 2016, Astronomical Society of Australia. This work has been 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 https://doi.org/10.1017/pasa.2016.56en
dc.subjectProtoplanetary disksen
dc.subjectMethods: observationalen
dc.subjectPlanets: formationen
dc.subjectAstronomical instrumentation, methods and techniquesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleA 'Rosetta Stone' for protoplanetary disks : the synergy of multi-wavelength observationsen
dc.typeJournal articleen
dc.description.versionPostprinten
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/10.1017/pasa.2016.56
dc.description.statusPeer revieweden
dc.date.embargoedUntil2017-06-13


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