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X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Wang, Pei1,2; Li, Jian3,4; Ji, Long5; Hou X(侯贤)6,7; Gügercinoğlu, Erbil1,8; Li, Di1,9,10; Torres, Diego F.11,12,13; Chen, Yutong1,14; Niu, Jiarui1,14; Zhu, Wei-Wei1,2; Zhang, Bing15; Liang, En-Wei16; Zhang, Li17; Ge, Mingyu18; Dai, Zigao3,4; Lin, Lin2; Han, Jinlin1; Feng, Yi10; Niu, Chenhui19; Zhang, Yongkun1,14; Zhou, Dejiang1,14; Xu, Heng1,20; Zhang, Chunfeng1,20; Jiang, Jinchen1,20; Miao, Chenchen10; Yuan, Mao21; Wang, Weiyang14,22; Zhou, Dengke10; Fang, Jianhua10; Yue, Youling1; Wu, Yunsheng23; Wang, Yabiao23; Wang, Chengjie23; Gan, Zhenye23; Li, Yuxi23; Sun, Zhongyi23; Chi, Mingmin24; Zhang, Junshuo1,14; Cao, Jinhuang1,14; Lu, Wanjin1,14; Wang, Yidan1,14
发表期刊ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
2024-12-01
卷号275期号:2
DOI10.3847/1538-4365/ad7c3f
产权排序第6完成单位
收录类别SCI
摘要Magnetars are neutron stars with extremely strong magnetic fields, frequently powering high-energy activity in X-rays. Pulsed radio emission following some X-ray outbursts has been detected, albeit its physical origin is unclear. It has long been speculated that the origin of magnetars' radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154's X-ray outburst and its associated fast radio burst 20200428, a radio pulsar phase was discovered. Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening.
资助项目MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[11988101]; MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[12041303]; National Natural Science Foundation of China (NSFC)[114-A11KYSB20160008]; CAS International Partnership Program[XDB23000000]; CAS Strategic Priority Research Program[2017YFA0402600]; National Key R&D Program of China[2020SKA0120200]; National SKA Program of China; CAS Youth Interdisciplinary Team[2021055]; Youth Innovation Promotion Association CAS; Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS[PID2021-124581OB-I00]; Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS[2021SGR00426]; Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS[CEX2020-001058-M]; Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS[EU PRTR-C17]; Spanish grants; Chinese Academy of Sciences
项目资助者MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[11988101, 12041303] ; National Natural Science Foundation of China (NSFC)[114-A11KYSB20160008] ; CAS International Partnership Program[XDB23000000] ; CAS Strategic Priority Research Program[2017YFA0402600] ; National Key R&D Program of China[2020SKA0120200] ; National SKA Program of China ; CAS Youth Interdisciplinary Team[2021055] ; Youth Innovation Promotion Association CAS ; Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS[PID2021-124581OB-I00, 2021SGR00426, CEX2020-001058-M, EU PRTR-C17] ; Spanish grants ; Chinese Academy of Sciences
语种英语
学科领域天文学 ; 射电与天文学
文章类型Article
出版者IOP Publishing Ltd
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0067-0049
URL查看原文
WOS记录号WOS:001366986400001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]SYNCHROTRON MASER EMISSION ; MAGNETAR PSR J1622-4950 ; GIANT PULSES ; BURSTS ; DISCOVERY ; OUTBURST ; ENVIRONMENT ; SAMPLE ; FLARE
引用统计
被引频次：1[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/27833
专题星系类星体研究组
中国科学院天体结构与演化重点实验室
作者单位1.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China; [email protected];
2.Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, People's Republic of China;
3.CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, People's Republic of China; [email protected];
4.School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, People's Republic of China;
5.School of Physics and Astronomy, Sun Yat-Sen University, Zhuhai, 519082, People's Republic of China;
6.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
7.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
8.Istanbul University, Faculty of Science, Department of Astronomy and Space Sciences, Beyazıt, 34119, Istanbul, Turkey;
9.Department of Astronomy, Tsinghua University, Beijing 100084, People's Republic of China;
10.Zhejiang Lab, Hangzhou, Zhejiang 311121, People's Republic of China;
11.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, 08193 Barcelona, Spain;
12.Institut d'Estudis Espacials de Catalunya (IEEC), 08860 Castelldefels (Barcelona), Spain;
13.Institució Catalana de Recerca i Estudis Avançats (ICREA), E-08010 Barcelona, Spain;
14.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China;
15.Department of Physics and Astronomy, University of Nevada, Las Vegas, Las Vegas, NV 89154, USA;
16.Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning 530004, People's Republic of China;
17.Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University, Kunming 650091, People's Republic of China;
18.Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China;
19.Institute of Astrophysics, Central China Normal University, Wuhan 430079, People's Republic of China;
20.Department of Astronomy, Peking University, Beijing 100871, People's Republic of China;
21.National Space Science Center, Chinese Academy of Sciences, Beijing 101400, People's Republic of China;
22.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China;
23.Tencent Youtu Lab, Shanghai 201103, People's Republic of China;
24.Fudan University, Shanghai 200438, People's Republic of China
推荐引用方式
GB/T 7714		 Wang, Pei,Li, Jian,Ji, Long,et al. X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2024,275(2).
APA Wang, Pei.,Li, Jian.,Ji, Long.,侯贤.,Gügercinoğlu, Erbil.,...&Wang, Yidan.(2024).X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,275(2).
MLA Wang, Pei,et al."X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 275.2(2024).
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