Details

Autor(en) / Beteiligte

• Yang, Zi-Xu
• Zhang, Liang
• Zhang, S N
• Méndez, M
• García, Federico
• Huang, Yue
• Bu, Qingcui
• Liu, He-Xin
• Yu, Wei
• Wang, P J
• Tao, L
• Altamirano, D
• Qu, Jin-Lu
• Zhang, S
• Ma, X
• Song, L M
• Jia, S M
• Ge, M Y
• Liu, Q Z
• Yan, J Z
• Li, T M
• Ren, X Q
• Ma, R C
• Zhang, Yuexin
• Xu, Y C
• Ma, B Y
• Du, Y F
• Fu, Y C
• Xiao, Y X
• Li, P P
• Jin, P
• Zhao, S J
• Zhao, Q C

Titel

Fast transitions of X-ray variability in the black hole transient GX 339−4: comparison with MAXI J1820+070 and MAXI J1348−630

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2023-03, Vol.521 (3), p.3570-3584

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2023

Link zum Volltext

Quelle

Free E-Journal (出版社公開部分のみ）

Beschreibungen/Notizen

• ABSTRACT Fast transitions between different types of power density spectra (PDS) happening over time-scales of several tens of seconds are rare phenomena in black hole X-ray binaries. In this paper, we report a broad-band spectral-timing analysis of the fast transitions observed in the 2021 outburst of GX 339−4 using NICER and Insight-HXMT observations. We observe transitions between band-limited noise-dominated PDS and type-B quasi-periodic oscillations (QPOs), and their rapid appearance or disappearance. We also make a detailed comparison between the fast transitions in GX 339−4 with those seen in MAXI J1820+070 and MAXI J1348−630. By comparing the spectra of the periods with and without type-B QPOs, we find that the spectral ratios above 10 keV are nearly constant or slightly decreasing, and the values are different between sources. Below 10 keV, the flux change of the Comptonization component is inversely proportional to the flux change of the thermal component, suggesting that the appearance of type-B QPOs is associated with a redistribution of the accretion power between the disc and the Comptonizing emission region. The spectral ratios between the periods with type-B QPO and those with broad-band noise are significantly different from that with type-B QPO and without type-B QPO, where the ratios (type-B QPO/broad-band noise) show a maximum at around 4 keV and then decrease gradually towards high energies. Finally, we discuss the possible change of the geometry of the inner accretion flow and/or jet during the transitions.