TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS
It has been suggested that chondrules and calcium-aluminum-rich inclusions (CAIs) were formed at the inner edge of the protoplanetary disk and then entrained in magnetocentrifugal X-winds. We study trajectories of such solid bodies with the consideration of the central star gravity, the protoplaneta...
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| Format: | Article |
| Language: | en_US |
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Institute of Physics/American Astronomical Society
2015
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| Online Access: | http://hdl.handle.net/1721.1/95840 |
| _version_ | 1811097206466281472 |
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| author | Hu, Renyu |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Hu, Renyu |
| author_sort | Hu, Renyu |
| collection | MIT |
| description | It has been suggested that chondrules and calcium-aluminum-rich inclusions (CAIs) were formed at the inner edge of the protoplanetary disk and then entrained in magnetocentrifugal X-winds. We study trajectories of such solid bodies with the consideration of the central star gravity, the protoplanetary disk gravity, and the gas drag of the wind. The efficiency of the gas drag depends on a parameter η, which is the product of the solid body size and density. We find that the gravity of the protoplanetary disk has a non-negligible effect on the trajectories. If a solid body re-enters the flared disk, the re-entering radius depends on the stellar magnetic dipole moment, the disk's gravity, the parameter η, and the initial launching angle. The disk's gravity can make the re-entering radius lower by up to 30%. We find a threshold η, denoted as η t , for any particular configuration of the X-wind, below which the solid bodies will be expelled from the planetary system. η t sensitively depends on the initial launching angle, and also depends on the mass of the disk. Only the solid bodies with an η larger than but very close to η t can be launched to a re-entering radius larger than 1 AU. This size-sorting effect may explain why chondrules come with a narrow range of sizes within each chondritic class. In general, the size distributions of CAIs and chondrules in chondrites can be determined from the initial size distribution as well as the distribution over the initial launching angle. |
| first_indexed | 2024-09-23T16:56:03Z |
| format | Article |
| id | mit-1721.1/95840 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T16:56:03Z |
| publishDate | 2015 |
| publisher | Institute of Physics/American Astronomical Society |
| record_format | dspace |
| spelling | mit-1721.1/958402022-09-29T22:29:27Z TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS Hu, Renyu Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Hu, Renyu It has been suggested that chondrules and calcium-aluminum-rich inclusions (CAIs) were formed at the inner edge of the protoplanetary disk and then entrained in magnetocentrifugal X-winds. We study trajectories of such solid bodies with the consideration of the central star gravity, the protoplanetary disk gravity, and the gas drag of the wind. The efficiency of the gas drag depends on a parameter η, which is the product of the solid body size and density. We find that the gravity of the protoplanetary disk has a non-negligible effect on the trajectories. If a solid body re-enters the flared disk, the re-entering radius depends on the stellar magnetic dipole moment, the disk's gravity, the parameter η, and the initial launching angle. The disk's gravity can make the re-entering radius lower by up to 30%. We find a threshold η, denoted as η t , for any particular configuration of the X-wind, below which the solid bodies will be expelled from the planetary system. η t sensitively depends on the initial launching angle, and also depends on the mass of the disk. Only the solid bodies with an η larger than but very close to η t can be launched to a re-entering radius larger than 1 AU. This size-sorting effect may explain why chondrules come with a narrow range of sizes within each chondritic class. In general, the size distributions of CAIs and chondrules in chondrites can be determined from the initial size distribution as well as the distribution over the initial launching angle. 2015-03-05T15:31:56Z 2015-03-05T15:31:56Z 2010-12 2010-02 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/95840 Hu, Renyu. “TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS.” The Astrophysical Journal 725, no. 2 (November 29, 2010): 1421–1428. © 2010 American Astronomical Society. en_US http://dx.doi.org/10.1088/0004-637x/725/2/1421 Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf Institute of Physics/American Astronomical Society American Astronomical Society |
| spellingShingle | Hu, Renyu TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title | TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title_full | TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title_fullStr | TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title_full_unstemmed | TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title_short | TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS |
| title_sort | transport of the first rocks of the solar system by x winds |
| url | http://hdl.handle.net/1721.1/95840 |
| work_keys_str_mv | AT hurenyu transportofthefirstrocksofthesolarsystembyxwinds |