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dc.contributor.authorLong, Feng
dc.contributor.authorPinilla, Paola
dc.contributor.authorHerczeg, Gregory J
dc.contributor.authorHarsono, Daniel
dc.contributor.authorDipierro, Giovanni
dc.contributor.authorPascucci, Ilaria
dc.contributor.authorHendler, Nathan
dc.contributor.authorTazzari, Marco
dc.contributor.authorRagusa, Enrico
dc.contributor.authorSalyk, Colette
dc.contributor.authorEdwards, Suzan
dc.contributor.authorLodato, Giuseppe
dc.contributor.authorPlas, Gerrit van de
dc.contributor.authorJohnstone, Doug
dc.contributor.authorLiu, Yao
dc.contributor.authorBoehler, Yann
dc.contributor.authorCabrit, Sylvie
dc.contributor.authorManara, Carlo F
dc.contributor.authorMenard, Francois
dc.contributor.authorMulders, Gijs D
dc.contributor.authorNisini, Brunella
dc.contributor.authorFischer, William J
dc.contributor.authorRigliaco, Elisabetta
dc.contributor.authorBanzatti, Andrea
dc.contributor.authorAvenhaus, Henning
dc.contributor.authorGully-Santiago, Michael
dc.date.accessioned2018-12-22T00:30:22Z
dc.date.available2018-12-22T00:30:22Z
dc.date.issued2018-12-10
dc.identifier.issn1538-4357
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/287364
dc.description.abstractRings are the most frequently revealed substructure in ALMA dust observations of protoplanetary disks, but their origin is still hotly debated. In this paper, we identify dust substructures in 12 disks and measure their properties to investigate how they form. This subsample of disks is selected from a high-resolution ($\sim0.12''$) ALMA 1.33 mm survey of 32 disks in the Taurus star-forming region, which was designed to cover a wide range of sub-mm brightness and to be unbiased to previously known substructures. While axisymmetric rings and gaps are common within our sample, spiral patterns and high contrast azimuthal asymmetries are not detected. Fits of disk models to the visibilities lead to estimates of the location and shape of gaps and rings, the flux in each disk component, and the size of the disk. The dust substructures occur across a wide range of stellar mass and disk brightness. Disks with multiple rings tend to be more massive and more extended. The correlation between gap locations and widths, the intensity contrast between rings and gaps, and the separations of rings and gaps could all be explained if most gaps are opened by low-mass planets (super-Earths and Neptunes) in the condition of low disk turbulence ($\alpha=10^{-4}$). The gap locations are not well correlated with the expected locations of CO and N$_2$ ice lines, so condensation fronts are unlikely to be a universal mechanism to create gaps and rings, though they may play a role in some cases.
dc.description.sponsorshipSeveral ERC grants.
dc.publisherIOP Publishing
dc.titleGaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region
dc.typeArticle
prism.number17
prism.publicationNameAstrophysical Journal
prism.volume869
dc.identifier.doi10.17863/CAM.34668
dcterms.dateAccepted2018-10-13
rioxxterms.versionofrecord10.3847/1538-4357/aae8e1
rioxxterms.versionAM
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2018-10-13
dc.contributor.orcidTazzari, Marco [0000-0003-3590-5814]
dc.identifier.eissn1538-4357
dc.publisher.urlhttp://dx.doi.org/10.3847/1538-4357/aae8e1
rioxxterms.typeJournal Article/Review
pubs.funder-project-idEuropean Research Council (341137)
cam.issuedOnline2018-12-06
cam.orpheus.successThu Jan 30 10:53:39 GMT 2020 - The item has an open VoR version.
rioxxterms.freetoread.startdate2100-01-01


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