Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios
The structure of dust aggregates affects many aspects of planet formation, such as the dust collision outcome, opacity, and radiation field. The millimeter-wave scattering polarization in protoplanerary disks indicates that dust aggregates have relatively compact structures with a volume-filling fac...
| 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/acb92b |
| _version_ | 1797701430117662720 |
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| author | Hidekazu Tanaka Ryoichi Anayama Ryo Tazaki |
| author_facet | Hidekazu Tanaka Ryoichi Anayama Ryo Tazaki |
| author_sort | Hidekazu Tanaka |
| collection | DOAJ |
| description | The structure of dust aggregates affects many aspects of planet formation, such as the dust collision outcome, opacity, and radiation field. The millimeter-wave scattering polarization in protoplanerary disks indicates that dust aggregates have relatively compact structures with a volume-filling factor ≳0.1. In this study, to explain such compact dust aggregates, we examined the compression of dust aggregates in sticking collisions with high mass ratios by performing a large number of N -body simulations of sequential dust collisions for a wide parameter range. Previous N -body simulations reported inefficient compression in equal-mass collisions between large dust aggregates. In contrast, we found that collisions with high mass ratios can compress the dust aggregate much more effectively. We also developed a new compression model that explains our results for sequential collisions with high mass ratios. Finally, we applied the new compression model to dust aggregates in protoplanetary disks and found a possible pathway to create relatively compact dust aggregates that explain the observed millimeter-wave scattering polarization. |
| first_indexed | 2024-03-12T04:36:33Z |
| format | Article |
| id | doaj.art-f132c8867ebe4bf1bd1ad59ac47ebe0c |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:36:33Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-f132c8867ebe4bf1bd1ad59ac47ebe0c2023-09-03T09:56:15ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194516810.3847/1538-4357/acb92bCompression of Dust Aggregates via Sequential Collisions with High Mass RatiosHidekazu Tanaka0https://orcid.org/0000-0001-9659-658XRyoichi Anayama1Ryo Tazaki2https://orcid.org/0000-0003-1451-6836Astronomical Institute, Graduate School of Science, Tohoku University , 6-3, Aramaki, Aoba-ku, Sendai 980-8578, Japan ; hidekazu@astr.tohoku.ac.jpAstronomical Institute, Graduate School of Science, Tohoku University , 6-3, Aramaki, Aoba-ku, Sendai 980-8578, Japan ; hidekazu@astr.tohoku.ac.jp; Mitsubishi Electric Software Corporation , 2-4-1, Hamamatsucho, Minato-ku, Tokyo 105-5129, JapanAstronomical Institute, Graduate School of Science, Tohoku University , 6-3, Aramaki, Aoba-ku, Sendai 980-8578, Japan ; hidekazu@astr.tohoku.ac.jp; Institute of Planetology and Astrophysics, Université Grenoble Alpes , F-38000, Grenoble, FranceThe structure of dust aggregates affects many aspects of planet formation, such as the dust collision outcome, opacity, and radiation field. The millimeter-wave scattering polarization in protoplanerary disks indicates that dust aggregates have relatively compact structures with a volume-filling factor ≳0.1. In this study, to explain such compact dust aggregates, we examined the compression of dust aggregates in sticking collisions with high mass ratios by performing a large number of N -body simulations of sequential dust collisions for a wide parameter range. Previous N -body simulations reported inefficient compression in equal-mass collisions between large dust aggregates. In contrast, we found that collisions with high mass ratios can compress the dust aggregate much more effectively. We also developed a new compression model that explains our results for sequential collisions with high mass ratios. Finally, we applied the new compression model to dust aggregates in protoplanetary disks and found a possible pathway to create relatively compact dust aggregates that explain the observed millimeter-wave scattering polarization.https://doi.org/10.3847/1538-4357/acb92bCircumstellar dustPlanet formationPlanetesimalsProtoplanetary disks |
| spellingShingle | Hidekazu Tanaka Ryoichi Anayama Ryo Tazaki Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios The Astrophysical Journal Circumstellar dust Planet formation Planetesimals Protoplanetary disks |
| title | Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios |
| title_full | Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios |
| title_fullStr | Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios |
| title_full_unstemmed | Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios |
| title_short | Compression of Dust Aggregates via Sequential Collisions with High Mass Ratios |
| title_sort | compression of dust aggregates via sequential collisions with high mass ratios |
| topic | Circumstellar dust Planet formation Planetesimals Protoplanetary disks |
| url | https://doi.org/10.3847/1538-4357/acb92b |
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