Planetesimal Formation by the Gravitational Instability of Dust Ring Structures
We investigate the gravitational instability (GI) of dust ring structures and the formation of planetesimals by their gravitational collapse. The normalized dispersion relation of a self-gravitating ring structure includes two parameters that are related to its width and line mass (the mass per unit...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ac9fd0 |
| _version_ | 1797697169780637696 |
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| author | Sanemichi Z. Takahashi Eiichiro Kokubo Shu-ichiro Inutsuka |
| author_facet | Sanemichi Z. Takahashi Eiichiro Kokubo Shu-ichiro Inutsuka |
| author_sort | Sanemichi Z. Takahashi |
| collection | DOAJ |
| description | We investigate the gravitational instability (GI) of dust ring structures and the formation of planetesimals by their gravitational collapse. The normalized dispersion relation of a self-gravitating ring structure includes two parameters that are related to its width and line mass (the mass per unit length). We survey these parameters and calculate the growth rate and wavenumber. Additionally, we investigate the formation of planetesimals by growth of the GI of the ring that is formed by the growth of the secular GI of the protoplanetary disk. We adopt a massive, dust-rich disk as a disk model. We find the range of radii for fragmentation by the ring GI as a function of the width of the ring. The innermost radius for the ring GI is smaller for a smaller ring width. We also determine the range of the initial planetesimal mass resulting from the fragmentation of the ring GI. Our results indicate that the planetesimal mass can be as large as 10 ^28 g at its birth after the fragmentation. It can be as low as about 10 ^25 g if the ring width is 0.1% of the ring radius, and the lower limit increases with the ring width. Furthermore, we obtain approximate formulae for the upper and lower limits of the planetesimal mass. We predict that the planetesimals formed by the ring GI have prograde rotations because of the Coriolis force acting on the contracting dust. This is consistent with the fact that many trans-Neptunian binaries exhibit prograde rotation. |
| first_indexed | 2024-03-12T03:36:25Z |
| format | Article |
| id | doaj.art-221af9e10a6e43a78a16f5b0dca5deab |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:36:25Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-221af9e10a6e43a78a16f5b0dca5deab2023-09-03T13:08:52ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01945212010.3847/1538-4357/ac9fd0Planetesimal Formation by the Gravitational Instability of Dust Ring StructuresSanemichi Z. Takahashi0https://orcid.org/0000-0003-3038-364XEiichiro Kokubo1https://orcid.org/0000-0002-5486-7828Shu-ichiro Inutsuka2https://orcid.org/0000-0003-4366-6518National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan ; sanemichi.takahashi@nao.ac.jpNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan ; sanemichi.takahashi@nao.ac.jpDepartment of Physics, Nagoya University , Furo-cho, Chikusa-ku, Nagoya, 464-8602 Aichi, JapanWe investigate the gravitational instability (GI) of dust ring structures and the formation of planetesimals by their gravitational collapse. The normalized dispersion relation of a self-gravitating ring structure includes two parameters that are related to its width and line mass (the mass per unit length). We survey these parameters and calculate the growth rate and wavenumber. Additionally, we investigate the formation of planetesimals by growth of the GI of the ring that is formed by the growth of the secular GI of the protoplanetary disk. We adopt a massive, dust-rich disk as a disk model. We find the range of radii for fragmentation by the ring GI as a function of the width of the ring. The innermost radius for the ring GI is smaller for a smaller ring width. We also determine the range of the initial planetesimal mass resulting from the fragmentation of the ring GI. Our results indicate that the planetesimal mass can be as large as 10 ^28 g at its birth after the fragmentation. It can be as low as about 10 ^25 g if the ring width is 0.1% of the ring radius, and the lower limit increases with the ring width. Furthermore, we obtain approximate formulae for the upper and lower limits of the planetesimal mass. We predict that the planetesimals formed by the ring GI have prograde rotations because of the Coriolis force acting on the contracting dust. This is consistent with the fact that many trans-Neptunian binaries exhibit prograde rotation.https://doi.org/10.3847/1538-4357/ac9fd0Gravitational instabilityProtoplanetary disksPlanet formationPlanetesimals |
| spellingShingle | Sanemichi Z. Takahashi Eiichiro Kokubo Shu-ichiro Inutsuka Planetesimal Formation by the Gravitational Instability of Dust Ring Structures The Astrophysical Journal Gravitational instability Protoplanetary disks Planet formation Planetesimals |
| title | Planetesimal Formation by the Gravitational Instability of Dust Ring Structures |
| title_full | Planetesimal Formation by the Gravitational Instability of Dust Ring Structures |
| title_fullStr | Planetesimal Formation by the Gravitational Instability of Dust Ring Structures |
| title_full_unstemmed | Planetesimal Formation by the Gravitational Instability of Dust Ring Structures |
| title_short | Planetesimal Formation by the Gravitational Instability of Dust Ring Structures |
| title_sort | planetesimal formation by the gravitational instability of dust ring structures |
| topic | Gravitational instability Protoplanetary disks Planet formation Planetesimals |
| url | https://doi.org/10.3847/1538-4357/ac9fd0 |
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