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dc.contributor.authorMacías, Enrique-
dc.contributor.authorEspaillat, Catherine C.-
dc.contributor.authorRibas, Álvaro-
dc.contributor.authorSchwarz, Kamber R.-
dc.contributor.authorAnglada, Guillem-
dc.contributor.authorOsorio, Mayra-
dc.contributor.authorCarrasco-González, Carlos-
dc.contributor.authorGómez Rivero, José Francisco-
dc.contributor.authorRobinson, Connor-
dc.date.accessioned2020-06-10T08:11:45Z-
dc.date.available2020-06-10T08:11:45Z-
dc.date.issued2018-
dc.identifierdoi: 10.3847/1538-4357/aad811-
dc.identifierissn: 1538-4357-
dc.identifier.citationAstrophysical Journal 865(1): 37 (2018)-
dc.identifier.urihttp://hdl.handle.net/10261/213948-
dc.description.abstractOur understanding of protoplanetary disks is rapidly departing from the classical view of a smooth, axisymmetric disk. This is in part thanks to the high angular resolution that (sub)millimeter observations can provide. Here, we present the combined results of Atacama Large Millimeter/submillimeter Array (ALMA) (0.9 mm) and Very Large Array (VLA) (7 mm) dust continuum observations toward the protoplanetary disk around the solar analog GM Aur. Both images clearly resolve the ∼35 au inner cavity. The ALMA observations also reveal a fainter disk that extends up to ∼250 au. We model our observations using two approaches: an analytical fit to the observed deprojected visibilities, and a physical disk model that fits the spectral energy distribution as well as the VLA and ALMA observations. Despite not being evident in the deconvolved images, the VLA and ALMA visibilities can only be fitted with two bright rings of radii ∼40 and ∼80 au. Our physical model indicates that this morphology is the result of an accumulation or trapping of large dust grains, probably due to the presence of two pressure bumps in the disk. Even though alternative mechanisms cannot be discarded, the multiple rings suggest that forming planets may have cleared at least two gaps in the disk. Finally, our analysis suggests that the inner cavity might display different sizes at 0.9 and 7 mm. This discrepancy could be caused by the presence of free-free emission close to the star at 7 mm, or by a more compact accumulation of the large dust grains at the edge of the cavity.© 2018. The American Astronomical Society. All rights reserved.-
dc.description.sponsorshipE.M., C.C.E., and A.R. acknowledge support from the National Science Foundation under CAREER grant Number AST-1455042 and the Sloan Foundation. G.A., M.O., and J.F.G. are supported by the MINECO (Spain) AYA2014-57369-C3 and AYA2017-84390-C2 grants (co-funded by FEDER).-
dc.languageeng-
dc.publisherIOP Publishing-
dc.relationMINECO/ICTI2013-2016/AYA2014-57369-C3-
dc.relationMINECO/ICTI2013-2016/AYA2017-84390-C2-
dc.relation.isversionofPostprint-
dc.rightsopenAccess-
dc.subjectPlanet-disk interactions-
dc.subjectProtoplanetary disks-
dc.subjectStars: individual (GM Aurigae)-
dc.subjectStars: pre-main sequence-
dc.subjectTechniques: interferometric-
dc.titleMultiple Rings in the Transitional Disk of GM Aurigae Revealed by VLA and ALMA-
dc.typeartículo-
dc.identifier.doihttp://dx.doi.org/10.3847/1538-4357/aad811-
dc.relation.publisherversionhttp://dx.doi.org/10.3847/1538-4357/aad811-
dc.date.updated2020-06-10T08:11:45Z-
dc.contributor.funderNational Science Foundation (US)-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderEuropean Commission-
dc.contributor.funderAlfred P. Sloan Foundation-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000879es_ES
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