黑洞候选EXO中的可变电离磁盘风1846-031

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黑洞候选EXO中的可变电离磁盘风1846-031

A variable ionized disk wind in the black-hole candidate EXO 1846-031

论文作者

Wang, Yanan, Ji, Long, Garcia, Javier A., Dauser, Thomas, Mendez, 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.

论文摘要

34年后，黑洞候选人Exo 1846-031在2019年再次爆发。我们研究了其在硬性中间体和柔软状态的频谱特性，该特性具有Nustar和Insight-HXMT。在两个光谱状态下检测到了反射成分，但可能起源于不同的照明光谱：在中间状态下，照明源归因于一种硬冠状成分，在其他X射线二进制文件中通常观察到，而在柔软的状态下，disk自我反射可能会产生。两种情况都支持EXO 1846-031作为〜40度的低倾斜度系统。在硬中间状态下，在〜7.2 keV处清楚地检测到吸收线，对应于高度离子磁盘风（logξ> 6.1），速度高达0.06c。同时，在X射线之前和之后已经检测到了准杂音无线电排放，这意味着该系统中磁盘风和喷气机的共存。另外，该源中观察到的风可能由磁力驱动。吸收线以软状态消失，狭窄的发射线在反射部分的顶部出现约6.7 keV，这可能是磁盘风的证据，但是需要具有较高光谱分辨率的数据来检查这一点。

After 34 years, 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 the disk self-irradiation. Both cases support EXO 1846-031 as a low inclination system of ~40 degrees. 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 up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the co-existence of disk winds and jets in this system. Additionally, the observed wind in this source is potentially driven by magnetic forces. 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 the higher spectral resolution are required to examine this.

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