The double-peaked type I X-ray bursts with different mass accretion rate and fuel composition
文献类型：期刊论文
| 作者 | Song, Liyu3; Liu, Helei3; Zhu, Chunhua3 ; Zhen, Guoqing3; Lu, Guoliang2; Xu, Renxin1,4
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| 刊名 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
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| 出版日期 | 2024-03-18 |
| 卷号 | 529期号:3页码:3103-3111 |
| 关键词 | nuclear reactions, nucleosynthesis, abundances stars: neutron X-rays: binaries X-rays: bursts |
| ISSN号 | 0035-8711 |
| DOI | 10.1093/mnras/stae709 |
| 产权排序 | 2 |
| 英文摘要 | Using the MESA code, we have carried out a detailed survey of the available parameter space for the double-peaked type I X-ray bursts. We find that the double-peaked structure appears at mass accretion rate <(M)over dot> in the range of similar to(4 - 8) x 10(-10) M-circle dot/yr when metallicity Z = 0.01, while in the range of similar to(4-8) x 10(-9) M-circle dot/yr(-1) when Z = 0.05. Calculations of the metallicity impact suggest that the double peaks will disappear when Z less than or similar to 0.005 for M-center dot=5x10(-10)M circle dot/yr(-1) and Z less than or similar to 0.04 for <(M)over dot> = 5 x 10(-9) M-circle dot/yr(-1). Besides, the impacts of base heating Q(b), as well as nuclear reaction waiting points: Mg-22, Si-26, S-30, Ar-34, Ni-56, Zn-60, Ge-64, Se-68, Kr-72 have been explored. The luminosity of the two peaks decreases as Q(b) increases. Se-68(p, gamma)Br-69 is the most sensitive reaction, the double peaks disappear assuming that Ni-56(p, gamma)Cu-57 and Ge-64(p, gamma)As-65 reaction rates have been underestimated by a factor of 100 and the Mg-22(alpha, p)Al-25 reaction rate has been overestimated by a factor of 100, which indicates that Mg-22, Ni-56, Ge-64, Se-68 are possibly the most important nuclear waiting points impedance in the thermonuclear reaction flow to explain the double-peaked bursts. Comparisons to the double-peaked bursts from 4U 1636-53 and 4U 1730-22 suggest that the nuclear origins of double-peaked type I X-ray bursts are difficult to explain the observed larger peak times (t(p, 1) greater than or similar to 4 s, t(p, 2) greater than or similar to 8 s) and smaller peak ratio(r(1, 2) less than or similar to 0.5). The composition of ashes from double-peaked bursts is very different from the single-peaked bursts especially for the heavier p-nuclei. |
| WOS关键词 | PHOTOSPHERIC RADIUS EXPANSION ; NEUTRON-STARS ; THERMONUCLEAR BURST ; MODELS ; MODULES ; DEPENDENCE ; STABILITY ; CODE |
| 资助项目 | National Natural Science Foundation of China[12263006] ; National Natural Science Foundation of China[U2031204] ; National Natural Science Foundation of China[12163005] ; National Natural Science Foundation of China[12373038] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region[2022A03013-3] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001189423300007 |
| 出版者 | OXFORD UNIV PRESS |
| 资助机构 | National Natural Science Foundation of China ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region |
| 源URL | [http://ir.xao.ac.cn/handle/45760611-7/6462]  |
| 专题 | 研究单元未命名 |
| 通讯作者 | Liu, Helei |
| 作者单位 | 1.Peking Univ, Dept Astron, Beijing 100871, Peoples R China 2.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Peoples R China 3.Xinjiang Univ, Sch Phys Sci & Technol, Urumqi 830046, Peoples R China 4.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China |
| 推荐引用方式 GB/T 7714 | Song, Liyu,Liu, Helei,Zhu, Chunhua,et al. The double-peaked type I X-ray bursts with different mass accretion rate and fuel composition[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2024,529(3):3103-3111. |
| APA | Song, Liyu,Liu, Helei,Zhu, Chunhua,Zhen, Guoqing,Lu, Guoliang,&Xu, Renxin.(2024).The double-peaked type I X-ray bursts with different mass accretion rate and fuel composition.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,529(3),3103-3111. |
| MLA | Song, Liyu,et al."The double-peaked type I X-ray bursts with different mass accretion rate and fuel composition".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 529.3(2024):3103-3111. |
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来源：新疆天文台
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