WEKO3
アイテム
{"_buckets": {"deposit": "f0d3fe32-a1ed-44e3-8b78-efb14bb36156"}, "_deposit": {"id": "52245", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "52245"}, "status": "published"}, "_oai": {"id": "oai:tsukuba.repo.nii.ac.jp:00052245", "sets": ["7642", "3076"]}, "item_5_biblio_info_6": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2018-10", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "6", "bibliographicPageStart": "108", "bibliographicVolumeNumber": "70", "bibliographic_titles": [{"bibliographic_title": "PASJ : publications of the Astronomical Society of Japan"}]}]}, "item_5_description_4": {"attribute_name": "抄録", "attribute_value_mlt": [{"subitem_description": "To what extent can the one-dimensional slim disk model reproduce the multi-dimensional results of global radiation-hydrodynamic simulations of super-Eddington accretion? With this question in mind, we perform a systematic simulation study of accretion flow onto a non-spinning black hole for a variety of black hole masses of (10–107) M⊙ and mass accretion rates of (1.4 × 102–5.6 × 103) LEdd/c2 (with LEdd and c being the Eddington luminosity and the speed of light). In order to adequately resolve large-scale outflow structure, we extensively expand a simulation box to cover the space of 3000 rS (with rS being the Schwarzschild radius), larger than those in most previous studies, so that we can put relatively large angular momentum on the gas injected from the outer simulation boundary. The adopted Keplerian radius, at which the centrifugal force balances the gravitational force, is rK = 300 rS. The injected mass first falls and is accumulated at around this radius and then slowly accretes toward the central black hole via viscosity. We simulate such accretion processes, taking inverse and bulk Compton scattering into account. The simulated accretion flow is in a quasi-steady state inside rqss ∼ 200 rS. Within this radius the flow properties are, on the whole, in good agreement with those described by the slim disk model except that the radial density profile of the underlying disk is much flatter, ρ ∝ r−0.73 (cf. ρ ∝ r−3/2 in the slim disk model), due probably to efficient convection. We find very weak outflow from inside r ∼ 200 rS, unlike the previous studies.", "subitem_description_type": "Abstract"}]}, "item_5_publisher_27": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "OXFORD UNIV PRESS"}]}, "item_5_relation_11": {"attribute_name": "DOI", "attribute_value_mlt": [{"subitem_relation_type_id": {"subitem_relation_type_id_text": "10.1093/pasj/psy110", "subitem_relation_type_select": "DOI"}}]}, "item_5_rights_12": {"attribute_name": "権利", "attribute_value_mlt": [{"subitem_rights": "© The Author(s) 2018. Published by Oxford University Press on behalf of the Astronomical Society of Japan."}]}, "item_5_select_15": {"attribute_name": "著者版フラグ", "attribute_value_mlt": [{"subitem_select_item": "author"}]}, "item_5_source_id_7": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0004-6264", "subitem_source_identifier_type": "ISSN"}]}, "item_5_source_id_9": {"attribute_name": "書誌レコードID", "attribute_value_mlt": [{"subitem_source_identifier": "AA1082896X", "subitem_source_identifier_type": "NCID"}]}, "item_creator": {"attribute_name": "著者", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "大須賀, 健"}, {"creatorName": "オオスガ, ケン", "creatorNameLang": "ja-Kana"}, {"creatorName": "OHSUGA, Ken", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "204056", "nameIdentifierScheme": "WEKO"}, {"nameIdentifier": "90386508", "nameIdentifierScheme": "e-Rad", "nameIdentifierURI": "https://nrid.nii.ac.jp/ja/nrid/1000090386508"}, {"nameIdentifier": "0000004156", "nameIdentifierScheme": "筑波大学研究者総覧", "nameIdentifierURI": "http://trios.tsukuba.ac.jp/researcher/0000004156"}]}, {"creatorNames": [{"creatorName": "Kitaki, Takaaki", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "214624", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Mineshige, Shin", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "214625", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Kawashima, Tomohisa", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "214626", "nameIdentifierScheme": "WEKO"}]}]}, "item_files": {"attribute_name": "ファイル情報", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_date", "date": [{"dateType": "Available", "dateValue": "2019-11-01"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "PASJ_70-6.pdf", "filesize": [{"value": "7.9 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_free", "mimetype": "application/pdf", "size": 7900000.0, "url": {"label": "PASJ_70-6", "url": "https://tsukuba.repo.nii.ac.jp/record/52245/files/PASJ_70-6.pdf"}, "version_id": "e4888638-7df4-4584-8a36-6f87acccda97"}]}, "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": "journal article", "resourceuri": "http://purl.org/coar/resource_type/c_6501"}]}, "item_title": "Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model"}]}, "item_type_id": "5", "owner": "1", "path": ["7642", "3076"], "permalink_uri": "http://hdl.handle.net/2241/00157673", "pubdate": {"attribute_name": "公開日", "attribute_value": "2019-09-10"}, "publish_date": "2019-09-10", "publish_status": "0", "recid": "52245", "relation": {}, "relation_version_is_last": true, "title": ["Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model"], "weko_shared_id": 5}
Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model
http://hdl.handle.net/2241/00157673
http://hdl.handle.net/2241/00157673ce0e8605-0be2-43f7-92f8-481130be3b33
名前 / ファイル | ライセンス | アクション |
---|---|---|
PASJ_70-6 (7.9 MB)
|
|
Item type | Journal Article(1) | |||||
---|---|---|---|---|---|---|
公開日 | 2019-09-10 | |||||
タイトル | ||||||
タイトル | Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model | |||||
言語 | ||||||
言語 | eng | |||||
資源タイプ | ||||||
資源 | http://purl.org/coar/resource_type/c_6501 | |||||
タイプ | journal article | |||||
著者 |
大須賀, 健
× 大須賀, 健× Kitaki, Takaaki× Mineshige, Shin× Kawashima, Tomohisa |
|||||
抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | To what extent can the one-dimensional slim disk model reproduce the multi-dimensional results of global radiation-hydrodynamic simulations of super-Eddington accretion? With this question in mind, we perform a systematic simulation study of accretion flow onto a non-spinning black hole for a variety of black hole masses of (10–107) M⊙ and mass accretion rates of (1.4 × 102–5.6 × 103) LEdd/c2 (with LEdd and c being the Eddington luminosity and the speed of light). In order to adequately resolve large-scale outflow structure, we extensively expand a simulation box to cover the space of 3000 rS (with rS being the Schwarzschild radius), larger than those in most previous studies, so that we can put relatively large angular momentum on the gas injected from the outer simulation boundary. The adopted Keplerian radius, at which the centrifugal force balances the gravitational force, is rK = 300 rS. The injected mass first falls and is accumulated at around this radius and then slowly accretes toward the central black hole via viscosity. We simulate such accretion processes, taking inverse and bulk Compton scattering into account. The simulated accretion flow is in a quasi-steady state inside rqss ∼ 200 rS. Within this radius the flow properties are, on the whole, in good agreement with those described by the slim disk model except that the radial density profile of the underlying disk is much flatter, ρ ∝ r−0.73 (cf. ρ ∝ r−3/2 in the slim disk model), due probably to efficient convection. We find very weak outflow from inside r ∼ 200 rS, unlike the previous studies. | |||||
書誌情報 |
PASJ : publications of the Astronomical Society of Japan 巻 70, 号 6, p. 108, 発行日 2018-10 |
|||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0004-6264 | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA1082896X | |||||
DOI | ||||||
識別子タイプ | DOI | |||||
関連識別子 | 10.1093/pasj/psy110 | |||||
権利 | ||||||
権利情報 | © The Author(s) 2018. Published by Oxford University Press on behalf of the Astronomical Society of Japan. | |||||
著者版フラグ | ||||||
値 | author | |||||
出版者 | ||||||
出版者 | OXFORD UNIV PRESS |