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X-Ray Emission Evolution of the Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 during the 2017-2018 Outburst Observed by the MAXI GSC
Sugizaki, Mutsumi1,2; Oeda, Motoki1; Kawai, Nobuyuki1; Mihara, Tatehiro3; Makishima, Kazuo3,4; Nakajima, Motoki5
2020-06-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume896Issue:2Pages:15
AbstractThis paper reports on the X-ray emission evolution of the ultraluminous Galactic X-ray pulsar Swift J0243.6+6124 during the giant outburst from 2017 October to 2018 January as observed by the MAXI GSC all-sky survey. The 2-30 keV light curve and the energy spectra confirm the source luminosityL(X)assuming an isotropic emission reached 2.5 x 10(39)erg s(-1), 10 times higher than the Eddington limit for a 1.4Mneutron star. When the source was luminous withL(X) greater than or similar to 0. 9 x 10(38)erg s(-1), it generally exhibited a negative correlation on a hardness-intensity diagram. However, two hardness ratios, a soft color (=4-10 keV/2-4 keV) and a hard color (=10-20 keV/4-10 keV), showed somewhat different behavior across a characteristic luminosity ofL(c) 5 x 10(38)erg s(-1). The soft color changed more than the hard color whenL(X) L-c, whereas the opposite was observed aboveL(c). The spectral change aboveL(c)was represented by a broad enhanced feature at similar to 6 keV on top of the canonical cutoff power-law continuum. The pulse profiles, derived daily, made the transition from a single-peak to a double-peak as the source brightened acrossL(c). These spectral and pulse-shape properties can be interpreted by a scenario in which the accretion columns on the neutron-star surface, producing the Comptonized X-ray emission, gradually became taller asL(X)increases. The broad 6 keV enhancement could be a result of cyclotron-resonance absorption at similar to 10 keV, corresponding to a surface magnetic fieldB(s) 1.1 x 10(12)G. The spin-frequency derivatives calculated with the Fermi GBM data showed a smooth positive correlation withL(X)up to the outburst peak, and its linear coefficient is comparable to those of typical Be binary pulsars whoseB(s)are (1-8) x 10(12)G. These results suggest that theB(s)of Swift J0243.6+6124 is a few times 10(12)G.
KeywordNeutron stars Binary pulsars Accretion High mass x-ray binary stars
Funding OrganizationMinistry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences
DOI10.3847/1538-4357/ab93c7
WOS KeywordSLIT CAMERA GSC ; NEUTRON-STARS ; ACCRETING PULSAR ; MAGNETIC-FIELD ; EXO 2030+375 ; LUMINOSITY ; ABSORPTION
Language英语
Funding ProjectMinistry of Education, Culture, Sports, Science and Technology (MEXT) of Japan[17H06362] ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences[XDA15052100]
Funding OrganizationMinistry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences ; Strategic Pioneer Program on Space Science, Chinese Academy of Sciences
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000545033900001
PublisherIOP PUBLISHING LTD
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Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/82878
Collection中国科学院国家天文台
Corresponding AuthorSugizaki, Mutsumi
Affiliation1.Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan
2.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China
3.RIKEN, High Energy Astrophys Lab, 2-1 Hirosawa, Wako, Saitama 3510198, Japan
4.Univ Tokyo, Kavli IPMU, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan
5.Nihon Univ, Sch Dent Matsudo, 2-870-1 Sakaecho Nishi, Matsudo, Chiba 1018308, Japan
Recommended Citation
GB/T 7714
Sugizaki, Mutsumi,Oeda, Motoki,Kawai, Nobuyuki,et al. X-Ray Emission Evolution of the Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 during the 2017-2018 Outburst Observed by the MAXI GSC[J]. ASTROPHYSICAL JOURNAL,2020,896(2):15.
APA Sugizaki, Mutsumi,Oeda, Motoki,Kawai, Nobuyuki,Mihara, Tatehiro,Makishima, Kazuo,&Nakajima, Motoki.(2020).X-Ray Emission Evolution of the Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 during the 2017-2018 Outburst Observed by the MAXI GSC.ASTROPHYSICAL JOURNAL,896(2),15.
MLA Sugizaki, Mutsumi,et al."X-Ray Emission Evolution of the Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 during the 2017-2018 Outburst Observed by the MAXI GSC".ASTROPHYSICAL JOURNAL 896.2(2020):15.
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