{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360285707160900352.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1016/j.icarus.2010.04.021"}},{"identifier":{"@type":"URI","@value":"https://api.elsevier.com/content/article/PII:S0019103510001788?httpAccept=text/xml"}},{"identifier":{"@type":"URI","@value":"https://api.elsevier.com/content/article/PII:S0019103510001788?httpAccept=text/plain"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1005.2536"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Planetary growth with collisional fragmentation and gas drag"}],"description":[{"notation":[{"@value":"As planetary embryos grow, gravitational stirring of planetesimals by embryos strongly enhances random velocities of planetesimals and makes collisions between planetesimals destructive. The resulting fragments are ground down by successive collisions. Eventually the smallest fragments are removed by the inward drift due to gas drag. Therefore, the collisional disruption depletes the planetesimal disk and inhibits embryo growth. We provide analytical formulae for the final masses of planetary embryos, taking into account planetesimal depletion due to collisional disruption. Furthermore, we perform the statistical simulations for embryo growth (which excellently reproduce results of direct $N$-body simulations if disruption is neglected). These analytical formulae are consistent with the outcome of our statistical simulations. Our results indicate that the final embryo mass at several AU in the minimum-mass solar nebula can reach about $\\sim 0.1$ Earth mass within $10^7$ years. This brings another difficulty in formation of gas giant planets, which requires cores with $\\sim 10$ Earth masses for gas accretion. However, if the nebular disk is 10 times more massive than the minimum-mass solar nebula and the initial planetesimal size is larger than 100 km, as suggested by some models of planetesimal formation, the final embryo mass reaches about 10 Earth masses at 3-4 AU. The enhancement of embryos' collisional cross sections by their atmosphere could further increase their final mass to form gas giant planets at 5-10 AU in the solar system."}]},{"notation":[{"@value":"Accepted for publication in Icarus"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1420282801208431232","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40422761"},{"@type":"NRID","@value":"1000040422761"},{"@type":"NRID","@value":"9000380461489"},{"@type":"NRID","@value":"9000242142272"},{"@type":"NRID","@value":"9000018566984"},{"@type":"NRID","@value":"9000004982891"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0069627"}],"foaf:name":[{"@value":"Hiroshi Kobayashi"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276169265664","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"00282814"},{"@type":"NRID","@value":"1000000282814"},{"@type":"NRID","@value":"9000004983063"},{"@type":"NRID","@value":"9000278499379"},{"@type":"NRID","@value":"9000250470939"},{"@type":"NRID","@value":"9000250471105"},{"@type":"NRID","@value":"9000290384175"},{"@type":"NRID","@value":"9000310000007"},{"@type":"NRID","@value":"9000340952563"},{"@type":"NRID","@value":"9000304623411"},{"@type":"NRID","@value":"9000272962239"},{"@type":"NRID","@value":"9000250177936"},{"@type":"NRID","@value":"9000239847767"},{"@type":"NRID","@value":"9000253257285"},{"@type":"NRID","@value":"9000401952082"},{"@type":"NRID","@value":"9000254740243"},{"@type":"NRID","@value":"9000278499344"},{"@type":"NRID","@value":"9000247076830"},{"@type":"NRID","@value":"9000272962289"},{"@type":"NRID","@value":"9000331449297"},{"@type":"NRID","@value":"9000365496875"},{"@type":"NRID","@value":"9000381496986"},{"@type":"NRID","@value":"9000360597544"},{"@type":"NRID","@value":"9000340952924"},{"@type":"NRID","@value":"9000254261859"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/hidekazu_tanaka"}],"foaf:name":[{"@value":"Hidekazu Tanaka"}]},{"@id":"https://cir.nii.ac.jp/crid/1380285707160900352","@type":"Researcher","foaf:name":[{"@value":"Alexander V. Krivov"}]},{"@id":"https://cir.nii.ac.jp/crid/1420845751138511744","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"30409718"},{"@type":"NRID","@value":"1000030409718"},{"@type":"NRID","@value":"9000004983140"},{"@type":"NRID","@value":"9000239848080"},{"@type":"NRID","@value":"9000018860314"},{"@type":"NRID","@value":"9000283741899"},{"@type":"NRID","@value":"9000283742634"},{"@type":"NRID","@value":"9000000195963"},{"@type":"NRID","@value":"9000254261858"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/satoshi_inaba"}],"foaf:name":[{"@value":"Satoshi Inaba"}]}],"contributor":[{"@id":"https://cir.nii.ac.jp/crid/1891428067621075203","@type":"Researcher","foaf:name":[{"@value":"Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany]"}]},{"@id":"https://cir.nii.ac.jp/crid/1891428067621075207","@type":"Researcher","foaf:name":[{"@value":"Hokkaido University [Sapporo, Japan]"}]},{"@id":"https://cir.nii.ac.jp/crid/1891428067621075201","@type":"Researcher","foaf:name":[{"@value":"Waseda University"}]},{"@id":"https://cir.nii.ac.jp/crid/1891428067621075204","@type":"Researcher","foaf:name":[{"@value":"Waseda University [Tokyo, Japan]"}]},{"@id":"https://cir.nii.ac.jp/crid/1890866215796592640","@type":"Researcher","foaf:name":[{"@value":"Peer, Hal"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00191035"}],"prism:publicationName":[{"@value":"Icarus"}],"dc:publisher":[{"@value":"Elsevier BV"}],"prism:publicationDate":"2010-10","prism:volume":"209","prism:number":"2","prism:startingPage":"836","prism:endingPage":"847"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["https://www.elsevier.com/tdm/userlicense/1.0/"],"url":[{"@id":"https://api.elsevier.com/content/article/PII:S0019103510001788?httpAccept=text/xml"},{"@id":"https://api.elsevier.com/content/article/PII:S0019103510001788?httpAccept=text/plain"}],"createdAt":"2010-05-12","modifiedAt":"2018-12-11","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Planetary%20Formation","dc:title":"Planetary Formation"},{"@id":"https://cir.nii.ac.jp/all?q=Earth%20and%20Planetary%20Astrophysics%20(astro-ph.EP)","dc:title":"Earth and Planetary Astrophysics (astro-ph.EP)"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=Collisional%20Physics","dc:title":"Collisional Physics"},{"@id":"https://cir.nii.ac.jp/all?q=%5BSDU%5D%20Sciences%20of%20the%20Universe%20%5Bphysics%5D","dc:title":"[SDU] Sciences of the Universe [physics]"},{"@id":"https://cir.nii.ac.jp/all?q=Origin%20Solar%20System","dc:title":"Origin Solar System"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Solar%20and%20Stellar%20Astrophysics","dc:title":"Astrophysics - Solar and Stellar Astrophysics"},{"@id":"https://cir.nii.ac.jp/all?q=%5BSDU%5DSciences%20of%20the%20Universe%20%5Bphysics%5D","dc:title":"[SDU]Sciences of the Universe [physics]"},{"@id":"https://cir.nii.ac.jp/all?q=Jovian%20planets","dc:title":"Jovian planets"},{"@id":"https://cir.nii.ac.jp/all?q=Planetesimals","dc:title":"Planetesimals"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20and%20Stellar%20Astrophysics%20(astro-ph.SR)","dc:title":"Solar and Stellar Astrophysics (astro-ph.SR)"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Earth%20and%20Planetary%20Astrophysics","dc:title":"Astrophysics - Earth and Planetary Astrophysics"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257042192640","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"21244011"},{"@type":"JGN","@value":"JP21244011"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-21244011/"}],"notation":[{"@language":"ja","@value":"惑星系円盤ダストの統合モデルの確立"},{"@language":"en","@value":"Construction of a comprehensive model of dust in exoplanetary systems"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050013861703889024","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Dispersion and shattering strength of rocky and frozen planetesimals studied by laboratory experiments and numerical simulations"}]},{"@id":"https://cir.nii.ac.jp/crid/1050575520346941440","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites"}]},{"@id":"https://cir.nii.ac.jp/crid/1050854065054354688","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"The Growth of Protoplanets via the Accretion of Small Bodies in Disks Perturbed by the Planetary Gravity"}]},{"@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/1360002216959744640","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Growth efficiency of dust aggregates through collisions with high mass ratios"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002216960286336","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"On the water delivery to terrestrial embryos by ice pebble accretion"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004232399121920","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"United theory of planet formation (i): Tandem regime"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004234658434688","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Evolution of extinction curves in galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004239675668864","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"From Planetesimal to Planet in Turbulent Disks. 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