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Your search keyword '"Guo, C.C."' showing total 8 results
Start Over Author "Guo, C.C." Database Supplemental Index
8 results on '"Guo, C.C."'

1. Constant cyclotron line energy in Hercules X–1 - Joint Insight-HXMT and NuSTAR observations

Author

Xiao, G.C., Ji, L., Staubert, R., Ge, M.Y., Zhang, S., Zhang, S.N., Santangelo, A., Ducci, L., Liao, J.Y., Guo, C.C., Li, X.B., Zhang, W., Qu, J.L., Lu, F.J., Li, T.P., Song, L.M., Xu, Y.P., Bu, Q.C., Cai, C., Cao, X.L., Chang, Z., Chen, G., Chen, L., Chen, T.X., Chen, Y.B., Chen, Y., Chen, Y.P., 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., Gungor, C., Guo, C.C., Han, D.W., Huang, Y., Huo, J., 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, W., Li, X., Li, X.F., Li, Y.G., Li, Z.W., Liang, X.H., Liu, C.Z., Liu, G.Q., Liu, H.W., Liu, X.J., Liu, Y.N., Lu, B., Lu, X.F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J.Y., Ou, G., Sai, N., Song, S.X., Sun, L., Tan, Y., Tao, L., 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., Wu, M., Xiong, S.L., Yang, J.W., Yang, S., Yang, Y.J., Yang, Y.J., Yin, Q.B., Yin, Q.Q., 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., Zhang, Y., Zhang, Y.F., Zhang, Y.J., Zhang, Z., Zhang, Z., Zhang, Z.L., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zhou, J.F., Zhu, Y., and Zhu, Y.X.

Abstract

The long-term evolution of the centroid energy of the CRSF in Her X-1 is still a mystery. We report a new measurement from a campaign between Insight-HXMT and NuSTARperformed in February 2018. Generally, the two satellites show well consistent results of timing and spectral properties. The joint spectral analysis confirms that the previously observed long decay phase has ended, and that the line energy instead keeps constant around 37.5keV after flux correction.

Published
2019
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2. Insight-HXMT insight into switch of the accretion mode: The case of the X-ray pulsar 4U 1901+03

Author

Tuo, Y.L., Ji, L., Tsygankov, S.S., Mihara, T., Song, L.M., Ge, M.Y., Nabizadeh, A., Tao, L., Qu, J.L., Zhang, Y., Zhang, S., Zhang, S.N., Bu, Q.C., Chen, L., Xu, Y.P., Cao, X.L., Chen, Y., Liu, C.Z., Cai, C., Chang, Z., Chen, G., Chen, T.X., Chen, Y.B., Chen, Y.P., 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., Guo, C.C., Han, D.W., Huang, Y., Huo, J., Jia, S.M., Jiang, L.H., Jiang, W.C., Jin, J., Jin, Y.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, B.S., Liu, G.Q., Liu, H.W., Liu, X.J., Liu, Y.N., Lu, B., Lu, F.J., Lu, X.F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J.Y., Ou, G., Sai, N., Shang, R.C., Song, X.Y., Sun, L., Tan, Y., Wang, C., Wang, G.F., Wang, 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, J.W., Yang, S., Yang, Y.J., Yang, Y.J., 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., Zhang, Y.F., Zhang, Y.J., Zhang, Y.H., Zhang, Y., Zhang, Z., Zhang, Z., Zhang, Z.L., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zheng, Y.G., Zhou, D.K., Zhou, J.F., Zhu, Y.X., Zhu, Y., and Zhuang, R.L.

Abstract

We use the Insight-HXMT data collected during the 2019 outburst from X-ray pulsar 4U 1901+03 to complement the orbital parameters reported by Fermi/GBM. Using the Insight-HXMT, we examine the correlation between the derivative of the intrinsic spin frequency and bolometric flux based on accretion torque models. It was found that the pulse profiles significantly evolve during the outburst. The existence of two types of the profile's pattern discovered in the Insight-HXMT data indicates that this source experienced transition between a super-critical and a sub-critical accretion regimes during its 2019 outburst. Based on the evolution of the pulse profiles and the torque model, we derive the distance to 4U 1901+03 as 12.4±0.2kpc.

Published
2020
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3. Diagnostic of the spectral properties of Aquila X-1 by Insight-HXMT snapshots during the early propeller phase

Author

Güngör, C., 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., Guo, C.C., 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., Wu, M., Xiao, G.C., Xiao, S., Xiong, S.L., Xu, Y.P., Yang, J.W., Yang, S., Yang, Y.J., 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., 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., and Zhu, Y.X.

Abstract

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 fast-rise-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.

Published
2020
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4. Insight-HXMT study of the timing properties of Sco X-1

Author

Jia, S.M., Bu, Q.C., Qu, J.L., Lu, F.J., Zhang, S.N., Huang, Y., Ma, X., Tao, L., Xiao, G.C., Zhang, W., Chen, L., Song, L.M., Zhang, S., Li, T.P., Xu, Y.P., Cao, X.L., Chen, Y., Liu, C.Z., Cai, C., Chang, Z., Chen, G., Chen, T.X., Chen, Y.B., Chen, Y.P., Cui, W., Cui, W.W., Deng, J.K., Dong, Y.W., Du, Y.Y., Fu, M.X., Gao, G.H., Gao, H., Gao, M., Ge, M.Y., Gu, Y.D., Guan, J., Guo, C.C., Han, D.W., Huo, J., Jiang, L.H., Jiang, W.C., Jin, J., Jin, Y.J., Kong, L.D., Li, B., Li, C.K., Li, G., Li, M.S., Li, W., Li, X., Li, X.B., Li, X.F., Li, Y.G., Li, Z.W., Liang, X.H., Liao, J.Y., Liu, G.Q., Liu, H.W., Liu, X.J., Liu, Y.N., Lu, B., 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., Tuo, Y.L., Wang, C., Wang, G.F., Wang, J., Wang, W.S., Wang, Y.S., Wen, X.Y., Wu, B.Y., Wu, B.B., Wu, M., Xiao, S., Xiong, S.L., Yang, J.W., Yang, S., Yang, Y.J., Yin, Q.Q., Yi, Q.B., You, Y., Zhang, A.M., Zhang, C.M., Zhang, F., Zhang, H.M., Zhang, J., Zhang, T., Zhang, W.C., Zhang, W.Z., Zhang, Y., Zhang, Y.F., Zhang, Y.J., Zhang, Y., Zhang, Z., Zhang, Z.L., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zhou, D.K., Zhou, J.F., Zhu, Y.X., Zhu, Y., and Zhuang, R.L.

Abstract

We present a detailed timing study of the brightest persistent X-ray source Sco X-1 using the data collected by the Hard X-ray Modulation Telescope (Insight-HXMT) from July 2017 to August 2018. A complete Z-track hardness-intensity diagram (HID) is obtained. The normal branch oscillations (NBOs) at ∼ 6 Hz in the lower part of the normal branch (NB) and the flare branch oscillations (FBOs) at ∼ 16 Hz in the beginning part of the flaring branch (FB) are found in observations with the Low Energy X-ray Telescope (LE) and the Medium Energy X-ray Telescope (ME) of Insight-HXMT, while the horizontal branch oscillations (HBOs) at ∼ 40 Hz and the kilohertz quasi-periodic oscillations (kHz QPOs) at ∼ 800 Hz are found simultaneously above 20 keV for the first time on the horizontal branch (HB) by the High Energy X-ray Telescope (HE) and ME. We find that for all types of the observed QPOs, the centroid frequencies are independent of energy, while the root mean square (rms) increases with energy; the centroid frequencies of both the HBOs and kHz QPOs increase along the Z-track from the top to the bottom of the HB; and the NBOs show soft phase lags increasing with energy. A continuous QPO transition from the FB to NB in ∼ 200 s are also detected. Our results indicate that the non-thermal emission is the origin of all types of QPOs, the innermost region of the accretion disk is non-thermal in nature, and the corona is nonhomogeneous geometrically.

Published
2020
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5. Joint analysis of energy and RMS spectra from MAXI J1535-571 with Insight-HXMT

Author

Kong, L.D., Zhang, S., Chen, Y.P., Ji, L., Zhang, S.N., Yang, Y.R., Tao, L., Ma, X., Qu, J.L., Lu, F.J., Bu, Q.C., Chen, L., Song, L.M., Li, T.P., Xu, Y.P., Cao, X.L., Chen, Y., Liu, C.Z., Cai, C., Chang, Z., Chen, G., Chen, T.X., 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., Ge, M.Y., Gu, Y.D., Guan, J., Guo, C.C., Han, D.W., Huang, Y., Huo, J., Jia, S.M., Jiang, L.H., Jiang, W.C., Jin, J., Li, B., Li, C.K., Li, G., Li, M.S., Li, W., Li, X., Li, X.B., Li, X.F., Li, Y.G., Li, Z.W., Liang, X.H., Liao, J.Y., Liu, G.Q., Liu, H.X., Liu, H.W., Liu, S.Z., Liu, X.J., Liu, Y.N., Lu, B., Lu, X.F., Luo, Q., Luo, T., 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, G.F., Wang, 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., Xu, H., Yang, J.W., Yang, S., Yang, Y.J., Yi, Q.B., You, Y., Zhang, A.M., Zhang, C.M., Zhang, F., Zhang, H.M., Zhang, J., Zhang, P., Zhang, T., Zhang, W., Zhang, W.C., Zhang, W.Z., Zhang, Y., Zhang, Y.F., Zhang, Y.J., Zhang, Y.H., Zhang, Y., Zhang, Z., Zhang, Z.L., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zheng, Y.G., Zhou, D.K., Zhou, J.F., Zhu, Y.X., and Zhu, Y.

Abstract

A new black hole X-ray binary (BHXRB) MAXI J1535-571 was discovered by MAXI during its outburst in 2017. Using observations taken by the first Chinese X-ray satellite, the Hard X-ray Modulation Telescope (dubbed as Insight-HXMT), we perform a joint spectral analysis (2-150 keV) in both energy and time domains. The energy spectra provide the essential input for probing the intrinsic Quasi-Periodic Oscillation (QPO) fractional rms spectra (FRS). Our results show that during the intermediate state, the energy spectra are in general consistent with those reported by Swift/XRT and NuSTAR. However, the QPO FRS become harder and the FRS residuals may suggest the presence of either an additional power-law component in the energy spectrum or a turn-over in the intrinsic QPO FRS at high energies.

Published
2020
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6. Insight-HXMT observation on 4U 1608–52: Evolving spectral properties of a bright type-I X-ray burst

Author

Chen, Y.P., Zhang, S., Zhang, S.N., Ji, L., Kong, L.D., Santangelo, A., Qu, J.L., Lu, F.J., Li, T.P., Song, L.M., Xu, Y.P., Cao, X.L., Chen, Y., Liu, C.Z., Bu, Q.C., Cai, C., Chang, Z., Chen, G., Chen, L., Chen, T.X., 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., Ge, M.Y., Gu, Y.D., Guan, J., Guo, C.C., Han, D.W., Huang, Y., Huo, J., Jia, S.M., Jiang, L.H., Jiang, W.C., Jin, J., Li, B., Li, C.K., Li, G., Li, M.S., Li, W., Li, X., Li, X.B., Li, X.F., Li, Y.G., Li, Z.W., Liang, X.H., Liao, J.Y., Liu, G.Q., Liu, H.W., Liu, X.J., Liu, Y.N., Lu, B., Lu, X.F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J.Y., Ou, G., Ren, X.Q., Sai, N., Sun, L., Tan, Y., Tao, L., Tuo, Y.L., Wang, C., Wang, G.F., Wang, 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, J.W., Yang, S., Yang, Y.J., Yang, Y.J., Yi, Q.B., Yin, Q.Q., You, Y., Zhang, A.M., Zhang, C.L., Zhang, C.M., Zhang, F., Zhang, H.M., Zhang, J., Zhang, T., Zhang, W.C., Zhang, W., Zhang, W.Z., Zhang, Yi., Zhang, Y.F., Zhang, Y.J., Zhang, Y., Zhang, Z., Zhang, Z.L., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zhou, D.K., Zhou, J.F., Zhu, Y., and Zhu, Y.X.

Abstract

The evidences for the influence of thermonuclear (type-I) X-ray bursts upon the surrounding environments in neutron star low-mass X-ray binaries (LMXB) were detected previously via spectral and timing analyses. Benefitting from a broad energy coverage of Insight-HXMT, we analyze one photospheric radius expansion (PRE) burst, and find an emission excess at soft X-rays. Our spectral analysis shows that, such an excess is not likely relevant to the disk reflection induced by the burst emission and can be attributed to an enhanced pre-burst/persistent emission. We find that the burst and enhanced persistent emissions sum up to exceed Eddington luminosity by ∼ 40 percentages. We speculate that the enhanced emission is from a region beyond the PRE radius, or through the Comptonization of the corona.

Published
2019
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8. Accretion torque reversals in GRO J1008-57 revealed by Insight-HXMT

Author

Wang, W., Tang, Y.M., Tuo, Y.L., Epili, P.R., Zhang, S.N., Song, L.M., Lu, F.J., Qu, J.L., Zhang, S., Ge, M.Y., Huang, Y., Li, B., Bu, Q.C., Cai, C., Cao, X.L., Chang, Z., Chen, L., Chen, T.X., Chen, Y.B., Chen, Y., 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., Huo, J., Jia, S.M., Jiang, W.C., Jin, J., Kong, L.D., Li, C.K., Li, G., Li, T.P., Li, W., Li, X., Li, X.B., Li, X.F., Li, Z.W., Liang, X.H., Liao, J.Y., Liu, B.S., Liu, C.Z., Liu, H.X., Liu, H.W., 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., Tao, 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., Xu, Y.P., Yang, R.J., Yang, S., Yang, J.J., Yang, Y.J., Yi, B.B., Yin, Q.Q., You, Y., Zhang, F., Zhang, H.M., Zhang, J., Zhang, P., Zhang, W., Zhang, W.C., Zhang, Y.F., Zhang, Y.H., Zhao, H.S., Zhao, X.F., Zheng, S.J., Zheng, Y.G., and Zhou, D.K.

Abstract

GRO J1008-57, as a Be/X-ray transient pulsar, is considered to have the highest magnetic field in known neutron star X-ray binary systems. Observational data of the X-ray outbursts in GRO J1008-57 from 2017 to 2020 were collected by the Insight-HXMT satellite. In this work, the spin period of the neutron star in GRO J1008-57 was determined to be about 93.28 seconds in August 2017, 93.22 seconds in February 2018, 93.25 seconds in June 2019 and 93.14 seconds in June 2020. GRO J1008-57 evolved in the spin-up process with a mean rate of −(2.10±0.05)×10−4s/d from 2009 – 2018, and turned into a spin down process with a rate of (6.7±0.6)×10−5s/d from Feb 2018 to June 2019. During the type II outburst of 2020, GRO J1008-57 had the spin-up torque again. During the torque reversals, the pulse profiles and continuum X-ray spectra did not change significantly, and the cyclotron resonant scattering feature around 80 keV was only detected during the outbursts in 2017 and 2020. Based on the observed mean spin-up rate, we estimated the inner accretion disk radius in GRO J1008-57 (about 1 - 2 times of the Alfvén radius) by comparing different accretion torque models of magnetic neutron stars. During the spin-down process, the magnetic torque should dominate over the matter accreting inflow torque, and we constrained the surface dipole magnetic field B≥6×1012G for the neutron star in GRO J1008-57, which is consistent with the magnetic field strength obtained by cyclotron line centroid energy.

Published
2021
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