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PhysRevD.103.063037.pdf | 3.73 MB | Adobe PDF | 見る/開く |
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DCフィールド | 値 | 言語 |
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dc.contributor.author | Shibata, Masaru | en |
dc.contributor.author | Kiuchi, Kenta | en |
dc.contributor.author | Fujibayashi, Sho | en |
dc.contributor.author | Sekiguchi, Yuichiro | en |
dc.contributor.alternative | 柴田, 大 | ja |
dc.contributor.alternative | 木内, 建太 | ja |
dc.date.accessioned | 2022-07-07T02:26:54Z | - |
dc.date.available | 2022-07-07T02:26:54Z | - |
dc.date.issued | 2021-03 | - |
dc.identifier.uri | http://hdl.handle.net/2433/274808 | - |
dc.description.abstract | We evolve high-mass disks of mass 15–50 M⊙ orbiting a 50 M⊙ spinning black hole in the framework of numerical relativity. Such high-mass systems could be an outcome during the collapse of rapidly rotating very massive stars. The massive disks are dynamically unstable to the so-called one-armed spiral-shape deformation with the maximum fractional density perturbation of δρ/ρ≳0.1, and hence, high-amplitude gravitational waves are emitted. The waveforms are characterized by an initial high-amplitude burst with the frequency of ∼40–50 Hz and the maximum amplitude of (1–10)×10⁻²² at the hypothetical distance of 100 Mpc and by a subsequent low-amplitude quasiperiodic oscillation. We illustrate that the waveforms in our models with a wide range of the disk mass resemble that of GW190521. We also point out that gravitational waves from rapidly rotating very massive stars can be the source for 3rd-generation gravitational-wave detectors for exploring the formation process of rapidly spinning high-mass black holes of mass ∼50–100 M⊙ in an early universe. | en |
dc.language.iso | eng | - |
dc.publisher | American Physical Society (APS) | en |
dc.rights | Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Open access publication funded by the Max Planck Society. | en |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | - |
dc.subject | Gravitational wave sources | en |
dc.subject | Accretion disk & black-hole plasma | en |
dc.subject | Numerical relativity | en |
dc.subject | Gravitation, Cosmology & Astrophysics | en |
dc.title | Alternative possibility of GW190521: Gravitational waves from high-mass black hole-disk systems | en |
dc.type | journal article | - |
dc.type.niitype | Journal Article | - |
dc.identifier.jtitle | Physical Review D | en |
dc.identifier.volume | 103 | - |
dc.identifier.issue | 6 | - |
dc.relation.doi | 10.1103/PhysRevD.103.063037 | - |
dc.textversion | publisher | - |
dc.identifier.artnum | 063037 | - |
dcterms.accessRights | open access | - |
datacite.awardNumber | 16H02183 | - |
datacite.awardNumber | 18H01213 | - |
datacite.awardNumber | 20H00158 | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16H02183/ | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-18H01213/ | - |
datacite.awardNumber.uri | https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-20H00158/ | - |
dc.identifier.pissn | 2470-0010 | - |
dc.identifier.eissn | 2470-0029 | - |
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 | 合体する中性子星連星からの重力波と電磁波放射に対する研究 | ja |
jpcoar.awardTitle | ショートガンマ線バーストの中心動力源と重力波に関する数値的研究 | ja |
jpcoar.awardTitle | 中性子星連星の合体からの電磁波と重力波の迅速な計算 | ja |
出現コレクション: | 学術雑誌掲載論文等 |
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