A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846–031

Creators: Wang, Yanan; Ji, Long; García, Javier A.; Dauser, Thomas; Méndez, Mariano; Mao, Junjie; Tao, L.; Altamirano, Diego; Maggi, Pierre; Zhang, S. N.; Ge, M. Y.; Zhang, L.; Qu, J. L.; Zhang, S.; Ma, X.; Lu, F. J.; Li, T. P.; Huang, Y.; Zheng, S. J.; Chang, Z.; Tuo, Y. L.; Song, L. M.; Xu, Y. P.; Chen, Y.; Liu, C. Z.; Bu, Q. C.; Cai, C.; Cao, X. L.; Chen, L.; Chen, T. X.; Chen, Y. P.; Cui, W. W.; Du, Y. Y.; Gao, G. H.; Gu, Y. D.; Guan, J.; Guo, C. C.; Han, D. W.; Huo, J.; Jia, S. M.; Jiang, W. C.; Jin, J.; Kong, L. D.; Li, B.; Li, C. K.; Li, G.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, H. W.; Liu, X. J.; Lu, X. F.; Luo, Q.; Luo, T.; Meng, B.; Nang, Y.; Nie, J. Y.; Ou, G.; Sai, N.; Shang, R. C.; Song, X. Y.; Sun, L.; Tan, Y.; Wang, W. S.; Wang, Y. D.; Wang, Y. S.; Wen, X. Y.; Wu, B. B.; Wu, B. Y.; Wu, M.; Xiao, G. C.; Xiao, S.; Xiong, S. L.; Yang, S.; Yang, Y. J.; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, F.; Zhang, H. M.; Zhang, J.; Zhang, W. C.; Zhang, W.; Zhang, Y. F.; Zhao, H. S.; Zhao, X. F.; Zhou, D. K.

Abstract

After 34 yr, the black hole candidate EXO 1846–031 went into outburst again in 2019. We investigate its spectral properties in the hard intermediate and the soft states with NuSTAR and Insight-HXMT. A reflection component has been detected in the two spectral states but possibly originating from different illumination spectra: in the intermediate state, the illuminating source is attributed to a hard coronal component, which has been commonly observed in other X-ray binaries, whereas in the soft state, the reflection is probably produced by disk self-irradiation. Both cases support EXO 1846–031 as a low-inclination system of ~40°. An absorption line is clearly detected at ~7.2 keV in the hard intermediate state, corresponding to a highly ionized disk wind (log} ξ > 6.1) with a velocity of up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the coexistence of disk winds and jets in this system. If only the high-flux segment of the NuSTAR observation is considered, the observed wind appears to be magnetically driven. The absorption line disappeared in the soft state and a narrow emission line appeared at ~6.7 keV on top of the reflection component, which may be evidence for disk winds, but data with higher spectral resolution are required to examine this.

Additional Information

© 2020. The American Astronomical Society. Received 2020 July 30; revised 2020 October 25; accepted 2020 October 26; published 2020 December 29. We are grateful to Timothy R. Kallman for help with xstar. We thank the anonymous referee for the helpful comments. This work made use of the data from the Insight-HXMT mission, a project funded by China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). The Insight-HXMT team gratefully acknowledges the support from the National Program on Key Research and Development Project (grant No. 2016YFA0400800) from the Minister of Science and Technology of China (MOST) and the Strategic Priority Research Program of the Chinese Academy of Sciences (grant No. XDB23040400). The authors thank the support from the National Natural Science Foundation of China under grant Nos. 11673023, 11733009, 11603037, 11973052, U1838201, U1838115, U1938103, and U1838202. Y.W. and L.Z. acknowledge support from the Royal Society Newton Funds. D.A. acknowledges support from the Royal Society. J.M. acknowledges the support from STFC (UK) through the University of Strathclyde UK APAP network grant ST/R000743/1. J.A.G. acknowledges support from NASA grant 80NSSC20K1238 and from the Alexander von Humboldt Foundation. Additionally, this work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Software: XSPEC (v12.11.1; Arnaud 1996), NuSTARDAS (v2.0.0), HXMTDAS (v2.02; Zhang et al. 2020).

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