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Authordc.contributor.authorPérez, Sebastián 
Authordc.contributor.authorDunhill, A. 
Authordc.contributor.authorCasassus Montero, Simón 
Authordc.contributor.authorRomán Asenjo, Pablo 
Authordc.contributor.authorSzulágyi, J. 
Authordc.contributor.authorFlores, C. 
Authordc.contributor.authorMarino Estay, Sebastián 
Authordc.contributor.authorMontesinos, Matías 
Admission datedc.date.accessioned2016-01-03T02:08:03Z
Available datedc.date.available2016-01-03T02:08:03Z
Publication datedc.date.issued2015
Cita de ítemdc.identifier.citationAstrophysical Journal Letters Volumen: 811 Número: 1 Número de artículo: L5 (2015)en_US
Identifierdc.identifier.issn2041-8205
Identifierdc.identifier.otherDOI: 10.1088/2041-8205/811/1/L5
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/136133
General notedc.descriptionArtículo de publicación ISIen_US
Abstractdc.description.abstractThe identification of on-going planet formation requires the finest angular resolutions and deepest sensitivities in observations inspired by state-of-the-art numerical simulations. Hydrodynamic simulations of planetdisk interactions predict the formation of circumplanetary disks (CPDs) around accreting planetary cores. These CPDs have eluded unequivocal detection –their identification requires predictions in CPD tracers. In this work, we aim to assess the observability of embedded CPDs with ALMA as features imprinted in the gas kinematics. We use 3D Smooth Particle Hydrodynamic (SPH) simulations of CPDs around 1 and 5 MJup planets at large stellocentric radii, in locally isothermal and adiabatic disks. The simulations are then connected with 3D radiative transfer for predictions in CO isotopologues. Observability is assessed by corrupting with realistic long baseline phase noise extracted from the recent HL Tau ALMA data. We find that the presence of a CPD produces distinct signposts: 1) compact emission separated in velocity from the overall circumstellar disk’s Keplerian pattern, 2) a strong impact on the velocity pattern when the Doppler shifted line emission sweeps across the CPD location, and 3) a local increase in the velocity dispersion. We test our predictions with a simulation tailored for HD 100546 –which has a reported protoplanet candidate. We find that the CPDs are detectable in all 3 signposts with ALMA Cycle 3 capabilities for both 1 and 5 MJup protoplanets, when embedded in an isothermal disken_US
Patrocinadordc.description.sponsorshipFONDECYT 3140601 1130949 1141175 3140634 Millennium Nucleus (Chilean Ministry of Economy) RC130007 ALMA-CONICYT 31120007 31120006 CONICYT-Gemini grant 32130007 BASAL PFB-06 CATA Anillo ACT-86 FONDEQUIP AIC-57 QUIMAL-130008en_US
Lenguagedc.language.isoenen_US
Publisherdc.publisherIOPen_US
Type of licensedc.rightsAtribución-NoComercial-SinDerivadas 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Keywordsdc.subjectProtoplanetary disksen_US
Títulodc.titlePlanet Formation Signposts: Observability of Circumplanetary Disks Via Gas Kinematicsen_US
Document typedc.typeArtículo de revista


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Atribución-NoComercial-SinDerivadas 3.0 Chile
Except where otherwise noted, this item's license is described as Atribución-NoComercial-SinDerivadas 3.0 Chile