The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations
The potential for planet formation of a circumstellar disk depends on the dust and gas reservoirs, which evolve as a function of the disk age. The Atacama Large Millimeter/submillimeter Array AGE-PRO Large Program has measured several disk properties across three star-forming regions of different ag...
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2025-01-01
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| author | Nicolás T. Kurtovic Matías Gárate Paola Pinilla Ke Zhang Giovanni P. Rosotti Rossella Anania Ilaria Pascucci Benoît Tabone Leon Trapman Dingshan Deng Miguel Vioque John Carpenter Lucas A. Cieza Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Dary A. Ruiz-Rodriguez James Miley Camilo González-Ruilova Estephani Torres-Villanueva Aleksandra Kuznetsova |
| author_facet | Nicolás T. Kurtovic Matías Gárate Paola Pinilla Ke Zhang Giovanni P. Rosotti Rossella Anania Ilaria Pascucci Benoît Tabone Leon Trapman Dingshan Deng Miguel Vioque John Carpenter Lucas A. Cieza Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Dary A. Ruiz-Rodriguez James Miley Camilo González-Ruilova Estephani Torres-Villanueva Aleksandra Kuznetsova |
| author_sort | Nicolás T. Kurtovic |
| collection | DOAJ |
| description | The potential for planet formation of a circumstellar disk depends on the dust and gas reservoirs, which evolve as a function of the disk age. The Atacama Large Millimeter/submillimeter Array AGE-PRO Large Program has measured several disk properties across three star-forming regions of different ages, and in this study, we compare the observational results to dust evolution simulations. Using DustPy for the dust evolution, and RADMC-3D for the radiative transfer, we ran a large grid of models spanning stellar masses of 0.25, 0.50, 0.75, and 1.0 M _⊙ , with different initial conditions, including: disk sizes, disk gas masses, and dust-to-gas ratio, and viscosity. Our models are performed assuming smooth, weakly, or strongly substructured disks, aiming to investigate if any observational trend can favor or exclude the presence of dust traps. The observed gas masses in the disks of the AGE-PRO sample are not reproducible with our models, which only consider viscous evolution with constant α , suggesting that additional physical mechanisms play a role in the evolution of the gas mass of disks. When comparing the dust continuum emission fluxes and sizes at 1.3 mm, we find that most of the disks in the AGE-PRO sample are consistent with simulations that have either weak or strong dust traps. The evolution of spectral index in the AGE-PRO sample is also suggestive of an unresolved population of dust traps. Future observations at high angular resolution are still needed to test several hypotheses that result from comparing the observations to our simulations, including that more massive disks in gas mass have the potential to form dust traps at larger disk radii. |
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| spelling | doaj-art-106daf12b3da4e878b78c203626b1dc12025-07-31T13:01:06ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-019891610.3847/1538-4357/add1d0The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO ObservationsNicolás T. Kurtovic0https://orcid.org/0000-0002-2358-4796Matías Gárate1https://orcid.org/0000-0001-6802-834XPaola Pinilla2https://orcid.org/0000-0001-8764-1780Ke Zhang3https://orcid.org/0000-0002-0661-7517Giovanni P. Rosotti4https://orcid.org/0000-0003-4853-5736Rossella Anania5https://orcid.org/0009-0004-8091-5055Ilaria Pascucci6https://orcid.org/0000-0001-7962-1683Benoît Tabone7https://orcid.org/0000-0002-1103-3225Leon Trapman8https://orcid.org/0000-0002-8623-9703Dingshan Deng9https://orcid.org/0000-0003-0777-7392Miguel Vioque10https://orcid.org/0000-0002-4147-3846John Carpenter11https://orcid.org/0000-0003-2251-0602Lucas A. Cieza12https://orcid.org/0000-0002-2828-1153Laura M. Pérez13https://orcid.org/0000-0002-1199-9564Carolina Agurto-Gangas14https://orcid.org/0000-0002-7238-2306Anibal Sierra15https://orcid.org/0000-0002-5991-8073Dary A. Ruiz-Rodriguez16https://orcid.org/0000-0003-3573-8163James Miley17https://orcid.org/0000-0002-1575-680XCamilo González-Ruilova18https://orcid.org/0000-0003-4907-189XEstephani Torres-Villanueva19https://orcid.org/0000-0001-9961-8203Aleksandra Kuznetsova20https://orcid.org/0000-0002-6946-6787Max Planck Institute for Extraterrestrial Physics , Giessenbachstrasse 1, D-85748 Garching, Germany ; kurtovic@mpe.mpg.de; Max-Planck-Institut fur Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, GermanyMax-Planck-Institut fur Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, GermanyMax-Planck-Institut fur Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, Germany; Mullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USADipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyLunar and Planetary Laboratory, The University of Arizona , Tucson, AZ 85721, USAUniversité Paris-Saclay , CNRS, Institut d’Astrophysique Spatiale, Orsay, FranceDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USALunar and Planetary Laboratory, The University of Arizona , Tucson, AZ 85721, USAEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany; Joint ALMA Observatory , Alonso de Córdova 3107, Vitacura, Santiago 763-0355, ChileJoint ALMA Observatory , Avenida Alonso de Córdova 3107, Vitacura, Santiago, ChileInstituto de Estudios Astrofísicos , Universidad Diego Portales, Av. Ejercito 441, Santiago, ChileDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileMullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UK; Departamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USADepartamento de Física, Universidad de Santiago de Chile , Av. Victor Jara 3659, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile , ChileInstituto de Estudios Astrofísicos , Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile , ChileDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USACenter for Computational Astrophysics, Flatiron Institute , 162 Fifth Avenue, New York, NY 10025, USAThe potential for planet formation of a circumstellar disk depends on the dust and gas reservoirs, which evolve as a function of the disk age. The Atacama Large Millimeter/submillimeter Array AGE-PRO Large Program has measured several disk properties across three star-forming regions of different ages, and in this study, we compare the observational results to dust evolution simulations. Using DustPy for the dust evolution, and RADMC-3D for the radiative transfer, we ran a large grid of models spanning stellar masses of 0.25, 0.50, 0.75, and 1.0 M _⊙ , with different initial conditions, including: disk sizes, disk gas masses, and dust-to-gas ratio, and viscosity. Our models are performed assuming smooth, weakly, or strongly substructured disks, aiming to investigate if any observational trend can favor or exclude the presence of dust traps. The observed gas masses in the disks of the AGE-PRO sample are not reproducible with our models, which only consider viscous evolution with constant α , suggesting that additional physical mechanisms play a role in the evolution of the gas mass of disks. When comparing the dust continuum emission fluxes and sizes at 1.3 mm, we find that most of the disks in the AGE-PRO sample are consistent with simulations that have either weak or strong dust traps. The evolution of spectral index in the AGE-PRO sample is also suggestive of an unresolved population of dust traps. Future observations at high angular resolution are still needed to test several hypotheses that result from comparing the observations to our simulations, including that more massive disks in gas mass have the potential to form dust traps at larger disk radii.https://doi.org/10.3847/1538-4357/add1d0Protoplanetary disksStellar accretion disksHydrodynamical simulations |
| spellingShingle | Nicolás T. Kurtovic Matías Gárate Paola Pinilla Ke Zhang Giovanni P. Rosotti Rossella Anania Ilaria Pascucci Benoît Tabone Leon Trapman Dingshan Deng Miguel Vioque John Carpenter Lucas A. Cieza Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Dary A. Ruiz-Rodriguez James Miley Camilo González-Ruilova Estephani Torres-Villanueva Aleksandra Kuznetsova The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations The Astrophysical Journal Protoplanetary disks Stellar accretion disks Hydrodynamical simulations |
| title | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations |
| title_full | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations |
| title_fullStr | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations |
| title_full_unstemmed | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations |
| title_short | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). VI. Comparison of Dust Evolution Models to AGE-PRO Observations |
| title_sort | alma survey of gas evolution of protoplanetary disks age pro vi comparison of dust evolution models to age pro observations |
| topic | Protoplanetary disks Stellar accretion disks Hydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/add1d0 |
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