Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud | |
Hou X(侯贤)5,6; Ge, M. Y.4; Ji, L.3; Zhang, S. N.2,4; You, Y.2,4; Tao, L.4; Zhang, S.4; Soria, R.2; Feng, H.1; Zhou M(周明)5,6 | |
刊名 | ASTROPHYSICAL JOURNAL |
2022-10-01 | |
卷号 | 938期号:2 |
ISSN号 | 0004-637X |
DOI | 10.3847/1538-4357/ac8c93 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | We present detailed timing and spectral analyses of the transient X-ray pulsar RX J0209.6-7427 in the Small Magellanic Cloud during its 2019 giant outburst. With a better known distance than most galactic X-ray pulsars, its peak luminosity is determined to be (1.11 +/- 0.06) x 10(39) erg s(-1); it is thus a bona fide pulsating ultraluminous X-ray source (PULX). Owing to the broad energy band of Insight-HXMT, its pulsed X-ray emission was detected from 1 keV up to the 130-180 keV band, which is the highest energy emission detected from any PULXs outside the Milky Way. This allows us to conclude that its main pulsed X-ray emission is from the fan beam of the accretion column, and its luminosity is thus intrinsic. We also estimate its magnetic field of (4.8-8.6) x 10(12) or (1.7-2.2) x 10(13) G, from its spin evolution or transition in the accretion column structure during the outburst; we suggest that the two values of the magnetic field strength correspond to the dipole and multipole magnetic fields of the neutron star, similar to the recent discovery in the Galactic PULX Swift J0243.6+6124. Therefore, the nature of the neutron star and its ULX emission can be understood within the current theoretical frame of accreting neutron stars. This may have implications for understanding the nature of those farther away extragalactic PULXs. |
学科主题 | 天文学 ; 天体物理学 ; 高能天体物理学 ; 星系与宇宙学 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
资助项目 | China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project[2021YFA0718500] ; Ministry of Science and Technology of China (MOST) ; National Natural Science Foundation of China[U1938103] ; National Natural Science Foundation of China[12041303] ; National Natural Science Foundation of China[U1938109] ; National Natural Science Foundation of China[U1838202] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[U1838115] ; National Natural Science Foundation of China[U1838104] ; National Natural Science Foundation of China[12073029] ; National Natural Science Foundation of China[U1838107] ; National Natural Science Foundation of China[U1938201] ; National Natural Science Foundation of China[U2038101] ; Light of West China Program of the CAS ; Guangdong Major Project of Basic and Applied Basic Research[2019B030302001] |
WOS关键词 | MAGNETIZED NEUTRON-STARS ; NUSTAR J095551+6940.8 ; ACCRETION LUMINOSITY ; PULSING ULXS ; DISCOVERY ; BINARY ; PARAMETERS ; DEPENDENCE ; OUTBURST ; DISK |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP Publishing Ltd |
WOS记录号 | WOS:000870859400001 |
资助机构 | China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project[2021YFA0718500] ; Ministry of Science and Technology of China (MOST) ; National Natural Science Foundation of China[U1938103, 12041303, U1938109, U1838202, U1838201, U1838115, U1838104, 12073029, U1838107, U1938201, U2038101] ; Light of West China Program of the CAS ; Guangdong Major Project of Basic and Applied Basic Research[2019B030302001] |
内容类型 | 期刊论文 |
版本 | 出版稿 |
源URL | [http://ir.ynao.ac.cn/handle/114a53/25608] |
专题 | 云南天文台_高能天体物理研究组 |
通讯作者 | Hou X(侯贤) |
作者单位 | 1.Department of Astronomy, Tsinghua University, Beijing 100084, People's Republic of China 2.University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, People's Republic of China; 3.School of Physics and Astronomy, Sun Yat-Sen University, Zhuhai 519082, People's Republic of China; 4.Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China zhangsn@ihep.ac.cn; 5.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China; 6.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China; xhou@ynao.ac.cn; |
推荐引用方式 GB/T 7714 | Hou X,Ge, M. Y.,Ji, L.,et al. Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud[J]. ASTROPHYSICAL JOURNAL,2022,938(2). |
APA | Hou X.,Ge, M. Y..,Ji, L..,Zhang, S. N..,You, Y..,...&Wang JC.(2022).Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud.ASTROPHYSICAL JOURNAL,938(2). |
MLA | Hou X,et al."Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud".ASTROPHYSICAL JOURNAL 938.2(2022). |
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