Identifying Anticyclonic Vortex Features Produced by the Rossby Wave Instability in Protoplanetary Disks

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dc.citation.articleNumber3en_US
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber867en_US
dc.contributor.authorHuang, Pinghuien_US
dc.contributor.authorIsella, Andreaen_US
dc.contributor.authorLi, Huien_US
dc.contributor.authorLi, Shengtaien_US
dc.contributor.authorJi, Jianghuien_US
dc.date.accessioned2019-01-08T15:37:42Zen_US
dc.date.available2019-01-08T15:37:42Zen_US
dc.date.issued2018en_US
dc.description.abstractSeveral nearby protoplanetary disks have been observed to display large-scale crescents in the (sub)millimeter dust continuum emission. One interpretation is that these structures correspond to anticyclonic vortices generated by the Rossby wave instability within the gaseous disk. Such vortices have local gas overdensities and are expected to concentrate dust particles with a Stokes number around unity. This process might catalyze the formation of planetesimals. Whereas recent observations showed that dust crescents are indeed regions where millimeter-size particles have abnormally high concentration relative to the gas and smaller grains, no observations have yet shown that the gas within the crescent region counterrotates with respect to the protoplanetary disk. Here we investigate the detectability of anticyclonic features through measurement of the line-of-sight component of the gas velocity obtained with ALMA. We carry out 2D hydrodynamic simulations and 3D radiative transfer calculations of a protoplanetary disk characterized by a vortex created by the tidal interaction with a massive planet. As a case study, the disk parameters are chosen to mimic the IRS 48 system, which has the most prominent crescent observed to date. We generate synthetic ALMA observations of both the dust continuum and 12CO emission around the frequency of 345 GHz. We find that the anticyclonic features of the vortex are weak but can be detected if both the source and the observational setup are properly chosen. We provide a recipe for maximizing the probability of detecting such vortex features and present an analysis procedure to infer their kinematic properties.en_US
dc.identifier.citationHuang, Pinghui, Isella, Andrea, Li, Hui, et al.. "Identifying Anticyclonic Vortex Features Produced by the Rossby Wave Instability in Protoplanetary Disks." <i>The Astrophysical Journal,</i> 867, (2018) IOP Publishing: https://doi.org/10.3847/1538-4357/aae317.en_US
dc.identifier.digitalHuang_2018en_US
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aae317en_US
dc.identifier.urihttps://hdl.handle.net/1911/104973en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsOriginal content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/3.0/en_US
dc.titleIdentifying Anticyclonic Vortex Features Produced by the Rossby Wave Instability in Protoplanetary Disksen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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