| Item type |
琉球大学リポジトリ登録用アイテムタイプ(1) |
| 公開日 |
2023-04-20 |
| タイトル |
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タイトル |
Evolution of equal mass binary bare quark stars in full general relativity: Could a supramassive merger remnant experience prompt collapse? |
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言語 |
en |
| 作成者 |
Zhou, Enping
Kiuchi, Kenta
Shibata, Masaru
Tsokaros, Antonios
Uryu, Koji
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| アクセス権 |
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|
アクセス権 |
open access |
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アクセス権URI |
http://purl.org/coar/access_right/c_abf2 |
| 権利情報 |
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言語 |
en |
|
権利情報 |
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. |
| 内容記述 |
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内容記述タイプ |
Abstract |
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内容記述 |
We have evolved mergers of equal-mass binary quark stars, the total mass of which is close to the mass shedding limit of uniformly rotating configurations, in fully general relativistic hydrodynamic simulations, aimed at investigating the postmerger outcomes. In particular, we have identified the threshold mass for prompt black hole formation after the merger, by tracing the minimum lapse function as well as the amount of ejected material during the merger simulation. A semianalytical investigation based on the angular momentum contained in the merger remnant is also performed to verify the results. For the equation of state considered in this work, the maximum mass of cold spherical configurations is 2.10 M⊙, the threshold mass is found between 3.05 and 3.10 M⊙. This result is consistent (with a quantitative error smaller than 1%) with the universal relation derived from the numerical results of symmetric binary neutron star mergers. Contrary to the neutron star case, the threshold mass is close to the mass shedding limit of uniformly rotating quark star. Consequently, we have found that binary quark stars with total mass corresponding to the long-lived supramassive remnant for neutron star case, could experience collapse to black hole within several times dynamical timescale, making quark stars as exceptions of the commonly accepted postmerger scenarios for binary neutron star mergers.We have suggested explanation for both the similarity and the difference, between quark stars and neutron stars. |
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言語 |
en |
| 出版者 |
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出版者 |
American Physical Society Sites |
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言語 |
en |
| 言語 |
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言語 |
eng |
| 資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_6501 |
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資源タイプ |
journal article |
| 出版タイプ |
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出版タイプ |
VoR |
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出版タイプResource |
http://purl.org/coar/version/c_970fb48d4fbd8a85 |
| 識別子 |
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|
識別子 |
https://doi.org/10.1103/PhysRevD.106.103030 |
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識別子タイプ |
DOI |
| 識別子 |
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|
識別子 |
https://journals.aps.org/prd/abstract/10.1103/PhysRevD.106.103030 |
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識別子タイプ |
URI |
| 収録物識別子 |
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収録物識別子タイプ |
EISSN |
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収録物識別子 |
2470-0029 |
| 収録物識別子 |
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収録物識別子タイプ |
PISSN |
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収録物識別子 |
2470-0010 |
| 収録物名 |
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収録物名 |
PHYSICAL REVIEW D |
|
言語 |
en |
| 書誌情報 |
巻 106,
号 10,
発行日 2022-11-15
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PhysRevD.106.103030.pdf (411 KB)
