WEKO3
アイテム
{"_buckets": {"deposit": "1f6ac41c-6766-4356-9de6-725b5a832c11"}, "_deposit": {"created_by": 4, "id": "6026", "owners": [4], "pid": {"revision_id": 0, "type": "depid", "value": "6026"}, "status": "published"}, "_oai": {"id": "oai:nipr.repo.nii.ac.jp:00006026", "sets": ["780"]}, "author_link": ["7996", "20257", "16340", "9923"], "item_1_biblio_info_14": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2003-03", "bibliographicIssueDateType": "Issued"}, "bibliographicPageEnd": "79", "bibliographicPageStart": "58", "bibliographicVolumeNumber": "16", "bibliographic_titles": [{"bibliographic_title": "Antarctic meteorite research"}]}]}, "item_1_creator_8": {"attribute_name": "著者名(英)", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Okazaki, Ryuji", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "9923", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Nagao, Keisuke", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "7996", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Imae, Naoya", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "20257", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Kojima, Hideyasu", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "16340", "nameIdentifierScheme": "WEKO"}]}]}, "item_1_description_1": {"attribute_name": "ページ属性", "attribute_value_mlt": [{"subitem_description": "P(論文)", "subitem_description_type": "Other"}]}, "item_1_description_12": {"attribute_name": "抄録(英)", "attribute_value_mlt": [{"subitem_description": "We have measured noble gases in three nakhlites from Antarctica, Yamato (Y) 000593, Y000749, and Y000802, by step-heating and total-melting methods.The trapped ^\u003c36\u003eAr/^\u003c84\u003eKr/^\u003c132\u003eXe ratios determined for the bulk samples are around 80/3/1, identical to those of Nakhla. The Yamato nakhlites also release noble gases showing high ^\u003c129\u003eXe/^\u003c132\u003eXe (up to 1.486) and low ^\u003c84\u003eKr/^\u003c132\u003eXe (~1.5) at 1000 and 1300 ℃, which is one of the most characteristic signatures of nakhlites. The low ^\u003c84\u003eKr/^\u003c132\u003eXe, as compared to that of the Mars atmosphere, suggests the presence of a fractionated Martian atmosphere.Cosmic-ray exposure ages based on cosmogenic ^\u003c21\u003eNe are 11.7, 11.9, and 13.0 Ma for Y000593, Y000749, and Y000802, respectively. This supports the pairing based on the mineralogical and petrographical similarities and the location of the finds. The average of the ^\u003c21\u003eNe exposure ages is 12.05±0.69 Ma. We also calculated an apparent ^\u003c81\u003eKr-Kr age as 11.8±1.0 Ma from cosmic-ray produced radioactive ^\u003c81\u003eKr and stable Kr isotopes from Y000593. The coincidence with the ^\u003c21\u003eNe exposure age indicates a short terrestrial age (\u003c0.04 Ma). Hence, the Mars ejection time, as calculated from the sum of the ^\u003c21\u003eNe exposure age and terrestrial age, is 12.1±0.7 Ma. Calculated K-Ar gas retention age for the Yamato nakhlites is 1.24±0.22 Ga. The ejection time and gas retention age are close to those of non-Antarctic nakhlites and Chassigny. This suggests that the Yamato nakhlites were ejected from Mars together with other nakhlites and Chassigny. Xenon isotopes are mixtures of Chassigny Xe, fission Xe, and the Mars atmosphere. High-temperature fractions (1000-1750℃) are enriched in the Mars atmosphere and fission Xe components, compared to lower temperature fractions. There are similarities in Xe isotopes between Y000749 and Y000802 showing excesses in ^\u003c129\u003eXe and ^\u003c136\u003eXe, whereas Y000593 has only small excesses. The release pattern of ^\u003c130\u003eXe for Y000593 is also diff", "subitem_description_type": "Other"}]}, "item_1_identifier_registration": {"attribute_name": "ID登録", "attribute_value_mlt": [{"subitem_identifier_reg_text": "10.15094/00006026", "subitem_identifier_reg_type": "JaLC"}]}, "item_1_publisher_22": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "National Institute of Polar Research"}]}, "item_1_source_id_13": {"attribute_name": "雑誌書誌ID", "attribute_value_mlt": [{"subitem_source_identifier": "AA11182426", "subitem_source_identifier_type": "NCID"}]}, "item_1_text_10": {"attribute_name": "著者所属(英)", "attribute_value_mlt": [{"subitem_text_language": "en", "subitem_text_value": "Laboratory for Earthquake Chemistry, University of Tokyo"}, {"subitem_text_language": "en", "subitem_text_value": "Laboratory for Earthquake Chemistry, University of Tokyo"}, {"subitem_text_language": "en", "subitem_text_value": "Antarctic Meteorite Research Center, National Institute of Polar Research"}, {"subitem_text_language": "en", "subitem_text_value": "Antarctic Meteorite Research Center, National Institute of Polar Research"}]}, "item_files": {"attribute_name": "ファイル情報", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_date", "date": [{"dateType": "Available", "dateValue": "2003-03-01"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "KJ00000040862.pdf", "filesize": [{"value": "2.3 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_6", "mimetype": "application/pdf", "size": 2300000.0, "url": {"label": "KJ00000040862", "url": "https://nipr.repo.nii.ac.jp/record/6026/files/KJ00000040862.pdf"}, "version_id": "c01ebba3-6b64-414a-bc5a-56f7d8329bb4"}]}, "item_keyword": {"attribute_name": "キーワード", "attribute_value_mlt": [{"subitem_subject": "Martian meteorite", "subitem_subject_scheme": "Other"}, {"subitem_subject": "trapped noble gas", "subitem_subject_scheme": "Other"}, {"subitem_subject": "cosmic-ray exposure age", "subitem_subject_scheme": "Other"}, {"subitem_subject": "terrestrial age", "subitem_subject_scheme": "Other"}, {"subitem_subject": "K-Ar gas retention age", "subitem_subject_scheme": "Other"}]}, "item_language": {"attribute_name": "言語", "attribute_value_mlt": [{"subitem_language": "eng"}]}, "item_resource_type": {"attribute_name": "資源タイプ", "attribute_value_mlt": [{"resourcetype": "departmental bulletin paper", "resourceuri": "http://purl.org/coar/resource_type/c_6501"}]}, "item_title": "Noble gas signatures of Antarctic nakhlites, Yamato (Y) 000593, Y000749, and Y000802", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Noble gas signatures of Antarctic nakhlites, Yamato (Y) 000593, Y000749, and Y000802"}]}, "item_type_id": "1", "owner": "4", "path": ["780"], "permalink_uri": "https://doi.org/10.15094/00006026", "pubdate": {"attribute_name": "公開日", "attribute_value": "2003-03-01"}, "publish_date": "2003-03-01", "publish_status": "0", "recid": "6026", "relation": {}, "relation_version_is_last": true, "title": ["Noble gas signatures of Antarctic nakhlites, Yamato (Y) 000593, Y000749, and Y000802"], "weko_shared_id": 4}
Noble gas signatures of Antarctic nakhlites, Yamato (Y) 000593, Y000749, and Y000802
https://doi.org/10.15094/00006026
https://doi.org/10.15094/00006026d26ec7f6-b373-470d-9706-d9a0d44787b8
名前 / ファイル | ライセンス | アクション |
---|---|---|
KJ00000040862 (2.3 MB)
|
Item type | 紀要論文(ELS) / Departmental Bulletin Paper(1) | |||||
---|---|---|---|---|---|---|
公開日 | 2003-03-01 | |||||
タイトル | ||||||
タイトル | Noble gas signatures of Antarctic nakhlites, Yamato (Y) 000593, Y000749, and Y000802 | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | Martian meteorite | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | trapped noble gas | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | cosmic-ray exposure age | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | terrestrial age | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | K-Ar gas retention age | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | departmental bulletin paper | |||||
ID登録 | ||||||
ID登録 | 10.15094/00006026 | |||||
ID登録タイプ | JaLC | |||||
ページ属性 | ||||||
内容記述タイプ | Other | |||||
内容記述 | P(論文) | |||||
著者名(英) |
Okazaki, Ryuji
× Okazaki, Ryuji× Nagao, Keisuke× Imae, Naoya× Kojima, Hideyasu |
|||||
著者所属(英) | ||||||
en | ||||||
Laboratory for Earthquake Chemistry, University of Tokyo | ||||||
著者所属(英) | ||||||
en | ||||||
Laboratory for Earthquake Chemistry, University of Tokyo | ||||||
著者所属(英) | ||||||
en | ||||||
Antarctic Meteorite Research Center, National Institute of Polar Research | ||||||
著者所属(英) | ||||||
en | ||||||
Antarctic Meteorite Research Center, National Institute of Polar Research | ||||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We have measured noble gases in three nakhlites from Antarctica, Yamato (Y) 000593, Y000749, and Y000802, by step-heating and total-melting methods.The trapped ^<36>Ar/^<84>Kr/^<132>Xe ratios determined for the bulk samples are around 80/3/1, identical to those of Nakhla. The Yamato nakhlites also release noble gases showing high ^<129>Xe/^<132>Xe (up to 1.486) and low ^<84>Kr/^<132>Xe (~1.5) at 1000 and 1300 ℃, which is one of the most characteristic signatures of nakhlites. The low ^<84>Kr/^<132>Xe, as compared to that of the Mars atmosphere, suggests the presence of a fractionated Martian atmosphere.Cosmic-ray exposure ages based on cosmogenic ^<21>Ne are 11.7, 11.9, and 13.0 Ma for Y000593, Y000749, and Y000802, respectively. This supports the pairing based on the mineralogical and petrographical similarities and the location of the finds. The average of the ^<21>Ne exposure ages is 12.05±0.69 Ma. We also calculated an apparent ^<81>Kr-Kr age as 11.8±1.0 Ma from cosmic-ray produced radioactive ^<81>Kr and stable Kr isotopes from Y000593. The coincidence with the ^<21>Ne exposure age indicates a short terrestrial age (<0.04 Ma). Hence, the Mars ejection time, as calculated from the sum of the ^<21>Ne exposure age and terrestrial age, is 12.1±0.7 Ma. Calculated K-Ar gas retention age for the Yamato nakhlites is 1.24±0.22 Ga. The ejection time and gas retention age are close to those of non-Antarctic nakhlites and Chassigny. This suggests that the Yamato nakhlites were ejected from Mars together with other nakhlites and Chassigny. Xenon isotopes are mixtures of Chassigny Xe, fission Xe, and the Mars atmosphere. High-temperature fractions (1000-1750℃) are enriched in the Mars atmosphere and fission Xe components, compared to lower temperature fractions. There are similarities in Xe isotopes between Y000749 and Y000802 showing excesses in ^<129>Xe and ^<136>Xe, whereas Y000593 has only small excesses. The release pattern of ^<130>Xe for Y000593 is also diff | |||||
雑誌書誌ID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA11182426 | |||||
書誌情報 |
Antarctic meteorite research 巻 16, p. 58-79, 発行日 2003-03 |
|||||
出版者 | ||||||
出版者 | National Institute of Polar Research |