X射线重新加工在用Insight-HXMT观察到的脉冲星GX 301-2中

论文标题

X射线重新加工在用Insight-HXMT观察到的脉冲星GX 301-2中

X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

论文作者

Ji, L., Doroshenko, V., Suleimanov, V., Santangelo, A., Orlandini, M., Liu, J., Ducci, L., Zhang, S. N., Nabizadeh, A., Gavran, D., Zhang, S., Ge, M. Y., Li, X. B., Tao, L., Bu, Q. C., Qu, J. L., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, T. X., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., 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. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. X., Liu, H. W., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, R. J., Yang, S., Yang, Yan-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W., Zhang, W. C., Zhang, Yi, Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K.

论文摘要

我们研究了2017 - 2019年使用Insight-HxMT/LE检测到的GX 301-2观察结果中的吸收和发射特征。在不同的轨道阶段，我们发现了明显的Fe Kalpha，Kbeta和Ni Kalpha系，以及Compton肩膀和Fe K-Shell吸收边缘。这些特征是由于X射线重新处理是由于辐射与周围吸积材料之间的相互作用引起的。根据铁线kalpha和kbeta的比率，我们推断出积聚材料处于低电离状态。我们发现依赖轨道依赖的局部吸收柱密度，该密度具有较大的价值和较强的可变性。我们解释了积聚环境和/或增生过程不稳定性的不均匀性的结果。另外，可变局部色谱柱密度与整个轨道的铁kalpha线的等效宽度相关，这表明中子恒星附近的积聚材料是球形分布的。

We investigate the absorption and emission features in observations of GX 301-2 detected with Insight-HXMT/LE in 2017-2019. At different orbital phases, we found prominent Fe Kalpha, Kbeta and Ni Kalpha lines, as well as Compton shoulders and Fe K-shell absorption edges. These features are due to the X-ray reprocessing caused by the interaction between the radiation from the source and surrounding accretion material. According to the ratio of iron lines Kalpha and Kbeta, we infer the accretion material is in a low ionisation state. We find an orbital-dependent local absorption column density, which has a large value and strong variability around the periastron. We explain its variability as a result of inhomogeneities of the accretion environment and/or instabilities of accretion processes. In addition, the variable local column density is correlated with the equivalent width of the iron Kalpha lines throughout the orbit, which suggests that the accretion material near the neutron star is spherically distributed.

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