{"_buckets": {"deposit": "bdcddda7-90a0-448d-b010-0d880c0ea02a"}, "_deposit": {"id": "23328", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "23328"}, "status": "published"}, "_oai": {"id": "oai:nagoya.repo.nii.ac.jp:00023328"}, "item_10_biblio_info_6": {"attribute_name": "\u66f8\u8a8c\u60c5\u5831", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2016-10-11", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "2", "bibliographicPageEnd": "65", "bibliographicPageStart": "65", "bibliographicVolumeNumber": "830", "bibliographic_titles": [{"bibliographic_title": "Astrophysical Journal"}]}]}, "item_10_description_4": {"attribute_name": "\u6284\u9332", "attribute_value_mlt": [{"subitem_description": "The formation of solid cores in giant planets of mass $\\sim 10\\,{M}_{\\oplus }$ is numerically simulated following the scenario of S\u00e1ndor et al. In this scenario, there are two convergence zones, corresponding to the outer and inner edges of the dead zone, where the torque exerted on planetary embryos by the gas nebula is zero. At the outer edge of the dead zone, anticyclonic vortices accumulate infalling dust aggregates, and planetary embryos are continuously formed in this scenario. We performed N-body simulations and show that massive objects of $\\simeq 10\\,{M}_{\\oplus }$ are formed in ~2.5 Myr, starting from the embryos. The largest object is formed at the inner convergence zone, although planetary embryos are placed at the outer convergence zone. This is due to the scattering of embryos from the outer to the inner convergence zone, and the shorter damping timescale of eccentricity at the inner convergence zone compared to the outer one. We varied the migration timescale due to the torque from gas by changing the gas surface density around the convergence zones. We found that there is a critical migration timescale below which $10\\,{M}_{\\oplus }$-sized objects are formed. Furthermore, we conducted simulations in which the gas surface density evolves according to viscous accretion. The largest object is also formed at the inner convergence zone irrespective of the strength of turbulence. Throughout the simulations, the location of the largest mass is the inner convergence zone. We confirmed that the formation timescale of a core of a Jovian planet can be explained in this scenario.", "subitem_description_type": "Abstract"}]}, "item_10_identifier_60": {"attribute_name": "URI", "attribute_value_mlt": [{"subitem_identifier_type": "DOI", "subitem_identifier_uri": "http://doi.org/10.3847/0004-637X/830/2/65"}, {"subitem_identifier_type": "HDL", "subitem_identifier_uri": "http://hdl.handle.net/2237/25522"}]}, "item_10_publisher_32": {"attribute_name": "\u51fa\u7248\u8005", "attribute_value_mlt": [{"subitem_publisher": "IOP publishing"}]}, "item_10_rights_12": {"attribute_name": "\u6a29\u5229", "attribute_value_mlt": [{"subitem_rights": "\u00a9 2016. The American Astronomical Society"}]}, "item_10_select_15": {"attribute_name": "\u8457\u8005\u7248\u30d5\u30e9\u30b0", "attribute_value_mlt": [{"subitem_select_item": "publisher"}]}, "item_10_source_id_7": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0004-637X", "subitem_source_identifier_type": "ISSN"}]}, "item_creator": {"attribute_name": "\u8457\u8005", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Sirono, Sin-iti"}], "nameIdentifiers": [{"nameIdentifier": "69116", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Katayama, Masahumi"}], "nameIdentifiers": [{"nameIdentifier": "69117", "nameIdentifierScheme": "WEKO"}]}]}, "item_files": {"attribute_name": "\u30d5\u30a1\u30a4\u30eb\u60c5\u5831", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_date", "date": [{"dateType": "Available", "dateValue": "2018-02-22"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "Sirono_2016_ApJ_830_65.pdf", "filesize": [{"value": "1.2 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_free", "mimetype": "application/pdf", "size": 1200000.0, "url": {"label": "Sirono_2016_ApJ_830_65.pdf", "url": "https://nagoya.repo.nii.ac.jp/record/23328/files/Sirono_2016_ApJ_830_65.pdf"}, "version_id": "719a175a-0991-4f7e-8ce1-05f8a2059cf7"}]}, "item_language": {"attribute_name": "\u8a00\u8a9e", "attribute_value_mlt": [{"subitem_language": "eng"}]}, "item_resource_type": {"attribute_name": "\u8cc7\u6e90\u30bf\u30a4\u30d7", "attribute_value_mlt": [{"resourcetype": "journal article", "resourceuri": "http://purl.org/coar/resource_type/c_6501"}]}, "item_title": "THE FORMATION OF CORES OF GIANT PLANETS AT CONVERGENCE ZONES OF PLANETARY MIGRATION", "item_titles": {"attribute_name": "\u30bf\u30a4\u30c8\u30eb", "attribute_value_mlt": [{"subitem_title": "THE FORMATION OF CORES OF GIANT PLANETS AT CONVERGENCE ZONES OF PLANETARY MIGRATION"}]}, "item_type_id": "10", "owner": "1", "path": ["488/489/490"], "permalink_uri": "http://hdl.handle.net/2237/25522", "pubdate": {"attribute_name": "\u516c\u958b\u65e5", "attribute_value": "2017-01-24"}, "publish_date": "2017-01-24", "publish_status": "0", "recid": "23328", "relation": {}, "relation_version_is_last": true, "title": ["THE FORMATION OF CORES OF GIANT PLANETS AT CONVERGENCE ZONES OF PLANETARY MIGRATION"], "weko_shared_id": null}