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We confirm that runaway growth is a dominant mode of planetary accretion in a three-dimensional system where orbits of planetesimals have inclinations. In runaway growth, larger planetesimals grow more rapidly than smaller ones and the mass ratio between them increases monotonically. On the other hand, in a two-dimensional system where all orbits are coplanar, we find that runaway growth does not occur. These results are explained by the simple analytical argument."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380011143863016705","@type":"Researcher","foaf:name":[{"@value":"Eiichiro Kokubo"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011143863016704","@type":"Researcher","foaf:name":[{"@value":"Shigeru Ida"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00191035"}],"prism:publicationName":[{"@value":"Icarus"}],"dc:publisher":[{"@value":"Elsevier BV"}],"prism:publicationDate":"1996-09","prism:volume":"123","prism:number":"1","prism:startingPage":"180","prism:endingPage":"191"},"reviewed":"false","dc:rights":["https://www.elsevier.com/tdm/userlicense/1.0/"],"url":[{"@id":"https://api.elsevier.com/content/article/PII:S0019103596901487?httpAccept=text/xml"},{"@id":"https://api.elsevier.com/content/article/PII:S0019103596901487?httpAccept=text/plain"}],"createdAt":"2002-09-17","modifiedAt":"2019-05-08","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050579057243577856","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002215949558272","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Resolution dependence of disruptive collisions between planetesimals in the gravity regime"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004231408138880","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Protoatmospheres and Surface Environment of Protoplanets"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004239673724032","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004239674955648","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Gravitational Instability of a Dust Layer Composed of Porous Silicate Dust Aggregates in a Protoplanetary Disk"}]},{"@id":"https://cir.nii.ac.jp/crid/1360005518594434432","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Influences of protoplanet-induced three-dimensional gas flow on pebble accretion"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285706412421760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285707160900352","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Planetary growth with collisional fragmentation and gas drag"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285708690613504","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Toward understanding the origin of asteroid geometries"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285709359623168","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"THE FATE OF PLANETESIMALS IN TURBULENT DISKS WITH DEAD ZONES. 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