Diagnostic of the spectral properties of Aquila X-1 by Insight-HXMT snapshots during the early propeller phase

Yazar
Guo, C. C.
Wu, M.
Xiao, G. C.
Xiao, S.
Xiong, S. L.
Xu, Y. P.
Yang, J. W.
Yang, S.
Yi, Q. B.
Yin, Q. Q.
You, Y.
Zhang, A. M.
Zhang, C. M.
Zhang, F.
Zhang, H. M.
Zhang, J.
Zhang, T.
Zhang, W.
Zhang, W. C.
Zhang, W. Z.
Zhang, Y. F.
Zhang, Y. J.
Zhang, Z.
Zhang, Z. L.
Zhao, H. S.
Zhao, X. F.
Zheng, S. J.
Zhou, D. K.
Zhou, J. F.
Zhu, Y.
Zhu, Y. X.
Gungor, Can
Ge, M. Y.
Zhang, S.
Santangelo, A.
Zhang, S. N.
Lu, F. J.
Zhang, Y.
Chen, Y. P.
Tao, L.
Yang, Y. J.
Bu, Q. C.
Cai, C.
Cao, X. L.
Chang, Z.
Chen, G.
Chen, L.
Chen, T. X.
Chen, Y.
Chen, Y. B.
Cui, W.
Cui, W. W.
Deng, J. K.
Dong, Y. W.
Du, Y. Y.
Fu, M. X.
Gao, G. H.
Gao, H.
Gao, M.
Gu, Y. D.
Guan, J.
Han, D. W.
Huang, Y.
Huo, J.
Ji, L.
Jia, S. M.
Jiang, L. H.
Jiang, W. C.
Jin, J.
Kong, L. D.
Li, B.
Li, C. K.
Li, G.
Li, M. S.
Li, T. P.
Li, W.
Li, X.
Li, X. B.
Li, X. F.
Li, Y. G.
Li, Z. W.
Liang, X. H.
Liao, J. Y.
Liu, C. Z.
Liu, G. Q.
Liu, H. W.
Liu, X. J.
Liu, Y. N.
Lu, B.
Lu, X. F.
Luo, T.
Luo, Q.
Ma, X.
Meng, B.
Nang, Y.
Nie, J. Y.
Ou, G.
Sai, N.
Song, L. M.
Song, X. Y.
Sun, L.
Tan, Y.
Tuo, Y. L.
Wang, C.
Wang, G. F.
Wang, J.
Wang, W. S.
Wang, Y. S.
Wen, X. Y.
Wu, B. B.
Wu, B. Y.
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Özet
We study the 2018 outburst of Aql X-1 via the monitor of all sky X-ray image (MAXI) data. We show that the outburst starting in February 2018 is a member of short-lowclass in the frame of outburst duration and the peak count rate although the outburst morphology is slightly different from the other fastrise-exponential-decay (FRED) type outbursts with a milder rising stage. We study the partial accretion in the weak propeller stage of Aql X-1 via the MAXI data of the 2018 outburst. We report on the spectral analysis of 3 observations of Aquila X-1 obtained by Insight - hard X-ray modulation telescope (Insight-HXMT) during the late decay stage of the 2018 outburst. We discuss that the data taken by Insight-HXMT is just after the transition to the weak propeller stage. Our analysis shows the necessity of a comptonization component to take into account the existence of an electron cloud resulting photons partly up-scattered. (C) 2019 Elsevier B.V. All rights reserved.
Bağlantı
http://hdl.handle.net/20.500.12627/67309
https://doi.org/10.1016/j.jheap.2019.12.001
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