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

Wang Y, Ji L, Garcia JA, Dauser T, Mendez M, Mao J, Tao L, Altamirano D, Maggi P, Zhang SN, Ge MY, Zhang L, Qu JL, Zhang SN, Ma X, Lu FJ, Li TP, Huang Y, Zheng SJ, Chang Z, Tuo YL, Song LM, Xu YP, Chen Y, Liu CZ, Bu QC, Cai C, Cao XL, Chen L, Chen TX, Chen YP, Cui WW, Du YY, Gao GH, Gu YD, Guan J, Guo CC, Han DW, Huo J, Jia SM, Jiang WC, Jin J, Kong LD, Li B, Li CK, Li G, Li W, Li X, Li XB, Li XF, Li ZW, Liang XH, Liao JY, Liu HW, Liu XJ, Lu XF, Luo Q, Luo T, Meng B, Nang Y, Nie JY, Ou G, Sai N, Shang RC, Song XY, Sun L, Tan Y, Wang WS, Wang YD, Wang YS, Wen XY, Wu BB, Wu BY, Wu M, Xiao GC, Xiao S, Xiong SL, Yang S, Yang YJ, Yi QB, Yin QQ, You Y, Zhang F, Zhang HM, Zhang J, Zhang WC, Zhang W, Zhang YF, Zhao HS, Zhao XF, Zhou DK (2020)

Publication Type: Journal article

Publication year: 2020

Journal

Astrophysical Journal American Astronomical Society

Book Volume: 906

Article Number: 11

Journal Issue: 1

DOI: 10.3847/1538-4357/abc55e

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.

Authors with CRIS profile

Thomas Dauser Dr.Karl-Remeis-Sternwarte Bamberg, Astronomisches Institut

Involved external institutions

Université de Strasbourg (UDS) FR France (FR) Eberhard Karls Universität Tübingen DE Germany (DE) California Institute of Technology (Caltech) US United States (USA) (US) Chinese Academy of Sciences (CAS) / 中国科学院 CN China (CN) Beijing Normal University CN China (CN) University of Southampton GB United Kingdom (GB) University of Groningen / Rijksuniversiteit Groningen NL Netherlands (NL) University of Strathclyde GB United Kingdom (GB) Tsinghua University CN China (CN)

How to cite

APA:

Wang, Y., Ji, L., Garcia, J.A., Dauser, T., Mendez, M., Mao, J.,... Zhou, D.K. (2020). A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846-031. Astrophysical Journal, 906(1). https://doi.org/10.3847/1538-4357/abc55e

MLA:

Wang, Yanan, et al. "A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846-031." Astrophysical Journal 906.1 (2020).

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