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| R-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar | |
Zhou, Xia1 ; Li, Ang2; Li, Bao-An3
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| 2021-03-01 | |
| Source Publication | ASTROPHYSICAL JOURNAL
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| ISSN | 0004-637X |
| Volume | 910Issue:1Pages:62 |
| Contribution Rank | 1 |
| Abstract | The nature of GW190814's secondary component m(2) of mass 2.50-2.67 M in the mass gap between the currently known maximum mass of neutron stars and the minimum mass of black holes is currently under hot debate. Among the many possibilities proposed in the literature, m(2) was suggested to be a superfast pulsar, while its r-mode stability against runaway gravitational radiation through the Chandrasekhar-Friedman-Schutz mechanism is still unknown. Previously, Fortin et al. constructed a sample of 33 unified equations of state using the same nuclear interactions from the crust to the core consistently; from that sample we use those equations that fulfill all currently known astrophysical and nuclear physics constraints to compare the minimum frequency required for m(2) to rotationally sustain a mass greater than 2.50 M with the critical frequency above which the r-mode instability occurs. We use two extreme damping models assuming that the crust is either perfectly rigid or elastic. Using the stability of 19 observed low-mass X-ray binaries as an indication that the rigid crust damping of the r-mode dominates within the models studied, we find that m(2) is r-mode-stable while rotating with a frequency higher than 870.2 Hz (0.744 times its Kepler frequency of 1169.6 Hz) as long as its temperature is lower than about 3.9 x 10(7) K, further supporting the proposal that GW190814's secondary component is a supermassive and superfast pulsar. |
| Keyword | Pulsars Neutron stars |
| DOI | 10.3847/1538-4357/abe538 |
| URL | 查看原文 |
| Indexed By | SCI |
| Language | 英语 |
| Funding Project | National SKA Program of China[2020SKA0120300] ; National Natural Science Foundation of China[11873040] ; National Natural Science Foundation of China[12033001] ; Youth Innovation Fund of Xiamen[3502Z20206061] ; CAS Light of West China Program[2019-XBQNXZ-B-016] ; Tianshan Youth Program[2018Q039] ; U.S. Department of Energy, Office of Science[DE-SC0013702] ; CUSTIPEN (China-U.S. Theory Institute for Physics with Exotic Nuclei) under the US Department of Energy[DE-SC0009971] |
| WOS Research Area | Astronomy & Astrophysics |
| WOS Subject | Astronomy & Astrophysics |
| WOS ID | WOS:000633354300001 |
| Publisher | IOP PUBLISHING LTD |
| Funding Organization | National SKA Program of China ; National Natural Science Foundation of China ; Youth Innovation Fund of Xiamen ; CAS Light of West China Program ; Tianshan Youth Program ; U.S. Department of Energy, Office of Science ; CUSTIPEN (China-U.S. Theory Institute for Physics with Exotic Nuclei) under the US Department of Energy |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/3950 |
| Collection | 射电天文研究室_脉冲星研究团组 |
| Corresponding Author | Li, Ang |
| Affiliation | 1.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China 2.Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China 3.Texas A&M Univ Commerce, Dept Phys & Astron, Commerce, TX 75429 USA |
| First Author Affilication | Xinjiang Astronomical Observatory, Chinese Academy of Sciences |
| Recommended Citation GB/T 7714 | Zhou, Xia,Li, Ang,Li, Bao-An. R-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar[J]. ASTROPHYSICAL JOURNAL,2021,910(1):62. |
| APA | Zhou, Xia,Li, Ang,&Li, Bao-An.(2021).R-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar.ASTROPHYSICAL JOURNAL,910(1),62. |
| MLA | Zhou, Xia,et al."R-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar".ASTROPHYSICAL JOURNAL 910.1(2021):62. |
| Files in This Item: | ||||||
| File Name/Size | DocType | Version | Access | License | ||
| Zhou-2021-R-mode Sta（1041KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-SA | View Application Full Text | |
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