Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall
There is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km planet building blocks) by the streaming instability (SI). We f...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adef46 |
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| author | Daniel Carrera Abigail Davenport Jacob B. Simon Hans Baehr Til Birnstiel Cassandra Hall David Rea Sebastian Markus Stammler |
| author_facet | Daniel Carrera Abigail Davenport Jacob B. Simon Hans Baehr Til Birnstiel Cassandra Hall David Rea Sebastian Markus Stammler |
| author_sort | Daniel Carrera |
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| description | There is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km planet building blocks) by the streaming instability (SI). We focus on a recent suggestion that early infall causes an “inflationary” phase in which dust grains are advected outward. We modified the DustPy code to build a 1D disk that includes dust evolution, infall, and heating and cooling sources. We ran six models and examined the implications for the SI, taking into account recent works on how the SI responds to external turbulence. In line with other works, we find that grains are advected outward, which leads to an “advection-condensation-drift” loop that greatly enhances the dust density at the water snowline. However, we do not see this process at the silicate line. Instead, we find a new pile up at the edge of the expanding disk. However, despite these localized enhancements, even a modest amount of turbulence ( α = 10 ^−3 ) leaves planetesimal formation far out of reach. The midplane dust-to-gas ratio is at least an order of magnitude below the SI threshold, even taking into account recent results on how dust coagulation boosts the SI. For planetesimals to form in the Class 0/I phase may require a way to transport angular momentum without turbulence (e.g., disk winds) or a non-SI mechanism to form planetesimals. |
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| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-231be7836da4488bb52c5e3fc621df3d2025-08-22T06:19:48ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0199013910.3847/1538-4357/adef46Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to InfallDaniel Carrera0https://orcid.org/0000-0001-6259-3575Abigail Davenport1Jacob B. Simon2https://orcid.org/0000-0002-3771-8054Hans Baehr3https://orcid.org/0000-0002-0880-8296Til Birnstiel4https://orcid.org/0000-0002-1899-8783Cassandra Hall5https://orcid.org/0000-0002-8138-0425David Rea6https://orcid.org/0000-0002-5000-2747Sebastian Markus Stammler7https://orcid.org/0000-0002-1589-1796Department of Astronomy, New Mexico State University , Las Cruces, NM 88001, USA ; dcarrera@gmail.comDepartment of Physics and Astronomy, Iowa State University , Ames, IA 50010, USADepartment of Physics and Astronomy, Iowa State University , Ames, IA 50010, USADepartment of Physics and Astronomy, The University of Georgia , Athens, GA 30602, USAUniversity Observatory , Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany; Max Planck Institute for Solar System Research , Justus-von-Liebig-Weg 3, Göttingen, 37077, GermanyDepartment of Physics and Astronomy, The University of Georgia , Athens, GA 30602, USADepartment of Physics and Astronomy, Iowa State University , Ames, IA 50010, USAUniversity Observatory , Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, GermanyThere is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km planet building blocks) by the streaming instability (SI). We focus on a recent suggestion that early infall causes an “inflationary” phase in which dust grains are advected outward. We modified the DustPy code to build a 1D disk that includes dust evolution, infall, and heating and cooling sources. We ran six models and examined the implications for the SI, taking into account recent works on how the SI responds to external turbulence. In line with other works, we find that grains are advected outward, which leads to an “advection-condensation-drift” loop that greatly enhances the dust density at the water snowline. However, we do not see this process at the silicate line. Instead, we find a new pile up at the edge of the expanding disk. However, despite these localized enhancements, even a modest amount of turbulence ( α = 10 ^−3 ) leaves planetesimal formation far out of reach. The midplane dust-to-gas ratio is at least an order of magnitude below the SI threshold, even taking into account recent results on how dust coagulation boosts the SI. For planetesimals to form in the Class 0/I phase may require a way to transport angular momentum without turbulence (e.g., disk winds) or a non-SI mechanism to form planetesimals.https://doi.org/10.3847/1538-4357/adef46Planet formationExoplanet formationProtoplanetary disks |
| spellingShingle | Daniel Carrera Abigail Davenport Jacob B. Simon Hans Baehr Til Birnstiel Cassandra Hall David Rea Sebastian Markus Stammler Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall The Astrophysical Journal Planet formation Exoplanet formation Protoplanetary disks |
| title | Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall |
| title_full | Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall |
| title_fullStr | Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall |
| title_full_unstemmed | Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall |
| title_short | Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall |
| title_sort | turbulence inhibits planetesimal formation in class 0 i disks subject to infall |
| topic | Planet formation Exoplanet formation Protoplanetary disks |
| url | https://doi.org/10.3847/1538-4357/adef46 |
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