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DCフィールド | 値 | 言語 |
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dc.contributor.author | Mizumoto, Misaki | en |
dc.contributor.author | Nomura, Mariko | en |
dc.contributor.author | Done, Chris | en |
dc.contributor.author | Ohsuga, Ken | en |
dc.contributor.author | Odaka, Hirokazu | en |
dc.contributor.alternative | 水本, 岬希 | ja |
dc.contributor.alternative | 野村, 真理子 | ja |
dc.contributor.alternative | 大須賀, 健 | ja |
dc.contributor.alternative | 小高, 裕和 | ja |
dc.date.accessioned | 2021-04-30T04:59:55Z | - |
dc.date.available | 2021-04-30T04:59:55Z | - |
dc.date.issued | 2020-05 | - |
dc.identifier.uri | http://hdl.handle.net/2433/262707 | - |
dc.description | 超巨大ブラックホールから吹く「風」の謎を解明. 京都大学プレスリリース. 2020-11-19. | ja |
dc.description.abstract | UltraFast Outflows (UFO) are observed in some active galactic nuclei (AGN), with blueshifted and highly ionised Fe-K absorption features. AGN typically have a UV bright accretion flow, so UV line driving is an obvious candidate for launching these winds. However this mechanism requires material with UV opacity, in apparent conflict with the observed high ionisation state of the wind. In this paper we synthesise the X-ray energy spectra resulting from different lines of sight through a state of the art radiation hydrodynamics UV line driven disc wind simulation. We demonstrate that there are some lines of sight which only intercept highly ionised and fast outflowing material. The cooler material required for the UV line driving acceleration is out of the line of sight, close to the disc, shielded from the X-rays by a failed wind. We fit these simulated wind spectra to data from the archetypal UFO source PG 1211+143 and show that they broadly reproduce the depth and velocity of the iron absorption lines seen. This directly demonstrates that UV line driving is a viable mechanism to launch even the fastest UFOs. We simulate microcalorimeter observations of this wind and show that their high energy resolution can resolve the detailed structure in the wind and recover the wind energetics when combined with models which correctly estimate the line formation radius of the wind. New data from microcalorimeters will pave the way for physical predictions of AGN wind feedback in cosmological simulations. | en |
dc.language.iso | eng | - |
dc.publisher | Oxford University Press (OUP) | en |
dc.rights | This article has been accepted for publication in 'Monthly Notices of the Royal Astronomical Society' © 2021 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. | en |
dc.subject | galaxies: active | en |
dc.subject | galaxies: Seyfert | en |
dc.subject | galaxies: individual: PG 1211+143 | en |
dc.subject | X-rays: galaxies | en |
dc.title | UV line driven disc wind as the origin of ultrafast outflows in AGN | en |
dc.type | journal article | - |
dc.type.niitype | Journal Article | - |
dc.identifier.jtitle | Monthly Notices of the Royal Astronomical Society | en |
dc.identifier.volume | 503 | - |
dc.identifier.issue | 1 | - |
dc.identifier.spage | 1442 | - |
dc.identifier.epage | 1458 | - |
dc.relation.doi | 10.1093/mnras/staa3282 | - |
dc.textversion | publisher | - |
dc.relation.url | https://www.kyoto-u.ac.jp/ja/research/research_results/2020/201119_1.html | - |
dcterms.accessRights | open access | - |
datacite.awardNumber | 17H01102 | - |
datacite.awardNumber | 16K05309 | - |
datacite.awardNumber | 18K03710 | - |
datacite.awardNumber | 18H04592 | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/ja/grant/KAKENHI-PROJECT-17H01102/ | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/ja/grant/KAKENHI-PROJECT-16K05309/ | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/ja/grant/KAKENHI-PROJECT-18K03710/ | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/ja/grant/KAKENHI-PUBLICLY-18H04592/ | - |
dc.identifier.pissn | 0035-8711 | - |
dc.identifier.eissn | 1365-2966 | - |
jpcoar.funderName | 日本学術振興会 | ja |
jpcoar.funderName | 日本学術振興会 | ja |
jpcoar.funderName | 日本学術振興会 | ja |
jpcoar.funderName | 日本学術振興会 | ja |
jpcoar.awardTitle | 理論シミュレーションで解明する巨大ブラックホールの起源 | ja |
jpcoar.awardTitle | X線観測と理論との比較によるコンパクト天体への質量降着とアウトフロー現象の研究 | ja |
jpcoar.awardTitle | 輻射磁気流体力学計算と輻射スペクトル計算で解明する超高光度X線源の起源 | ja |
jpcoar.awardTitle | 連星ブラックホール形成の解明に向けた孤立ブラックホールの輻射磁気流体力学計算 | ja |
jpcoar.funderName.alternative | Japan Society for the Promotion of Science (JSPS) | en |
jpcoar.funderName.alternative | Japan Society for the Promotion of Science (JSPS) | en |
jpcoar.funderName.alternative | Japan Society for the Promotion of Science (JSPS) | en |
jpcoar.funderName.alternative | Japan Society for the Promotion of Science (JSPS) | en |
出現コレクション: | 学術雑誌掲載論文等 |
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