Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk
Abstract We investigate the effect of a radial pressure bump in a protoplanetary disk on planetesimal formation. We performed the two-dimensional numerical simulation of the dynamical interaction of solid particles and gas with an initially defined pressure bump under the assumption of axisymmetry....
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| Format: | Article |
| Language: | English |
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SpringerOpen
2017-04-01
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| Series: | Earth, Planets and Space |
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| Online Access: | http://link.springer.com/article/10.1186/s40623-017-0637-z |
| _version_ | 1818134164485963776 |
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| author | Isamu K. Onishi Minoru Sekiya |
| author_facet | Isamu K. Onishi Minoru Sekiya |
| author_sort | Isamu K. Onishi |
| collection | DOAJ |
| description | Abstract We investigate the effect of a radial pressure bump in a protoplanetary disk on planetesimal formation. We performed the two-dimensional numerical simulation of the dynamical interaction of solid particles and gas with an initially defined pressure bump under the assumption of axisymmetry. The aim of this work is to elucidate the effects of the stellar vertical gravity that were omitted in a previous study. Our results are very different from the previous study, which omitted the vertical gravity. Because dust particles settle toward the midplane because of the vertical gravity to form a thin dust layer, the regions outside of the dust layer are scarcely affected by the back-reaction of the dust. Hence, the gas column density keeps its initial profile with a bump, and dust particles migrate toward the bump. In addition, the turbulence due to the Kelvin–Helmholtz instability caused by the difference of the azimuthal velocities between the inside and outside of the dust layer is suppressed where the radial pressure gradient is reduced by the pressure bump. The dust settling proceeds further where the turbulence is weak, and a number of dust clumps are formed. The dust density in some clumps exceeds the Roche density. Planetesimals are considered to be formed from these clumps owing to the self-gravity. Graphical abstract . |
| first_indexed | 2024-12-11T09:04:16Z |
| format | Article |
| id | doaj.art-60423d451aa447cfb8832a219df548fa |
| institution | Directory Open Access Journal |
| issn | 1880-5981 |
| language | English |
| last_indexed | 2024-12-11T09:04:16Z |
| publishDate | 2017-04-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | Earth, Planets and Space |
| spelling | doaj.art-60423d451aa447cfb8832a219df548fa2022-12-22T01:13:40ZengSpringerOpenEarth, Planets and Space1880-59812017-04-016911610.1186/s40623-017-0637-zPlanetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary diskIsamu K. Onishi0Minoru Sekiya1Department of Earth and Planetary Sciences, Graduate School of Science, Kyushu UniversityDepartment of Earth and Planetary Sciences, Faculty of Science, Kyushu UniversityAbstract We investigate the effect of a radial pressure bump in a protoplanetary disk on planetesimal formation. We performed the two-dimensional numerical simulation of the dynamical interaction of solid particles and gas with an initially defined pressure bump under the assumption of axisymmetry. The aim of this work is to elucidate the effects of the stellar vertical gravity that were omitted in a previous study. Our results are very different from the previous study, which omitted the vertical gravity. Because dust particles settle toward the midplane because of the vertical gravity to form a thin dust layer, the regions outside of the dust layer are scarcely affected by the back-reaction of the dust. Hence, the gas column density keeps its initial profile with a bump, and dust particles migrate toward the bump. In addition, the turbulence due to the Kelvin–Helmholtz instability caused by the difference of the azimuthal velocities between the inside and outside of the dust layer is suppressed where the radial pressure gradient is reduced by the pressure bump. The dust settling proceeds further where the turbulence is weak, and a number of dust clumps are formed. The dust density in some clumps exceeds the Roche density. Planetesimals are considered to be formed from these clumps owing to the self-gravity. Graphical abstract .http://link.springer.com/article/10.1186/s40623-017-0637-zPlanetary systemsProtoplanetary disksSolar system formationHydrodynamicsInstabilitiesPlanetesimal |
| spellingShingle | Isamu K. Onishi Minoru Sekiya Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk Earth, Planets and Space Planetary systems Protoplanetary disks Solar system formation Hydrodynamics Instabilities Planetesimal |
| title | Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| title_full | Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| title_fullStr | Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| title_full_unstemmed | Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| title_short | Planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| title_sort | planetesimal formation by an axisymmetric radial bump of the column density of the gas in a protoplanetary disk |
| topic | Planetary systems Protoplanetary disks Solar system formation Hydrodynamics Instabilities Planetesimal |
| url | http://link.springer.com/article/10.1186/s40623-017-0637-z |
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