Accretion Scenario of MAXI J1820+070 during 2018 Outbursts with Multi-mission Observations

Abstract

We present a comprehensive spectral and temporal study of the black hole X-ray transient MAXI J1820+070 during its outbursts in 2018 using Swift/XRT, NICER, NuSTAR and AstroSat observations. The Swift/XRT and NICER spectral study shows a plateau in the light curve with spectral softening (hardness changes from ∼ 2.5 to 2) followed by a gradual decline without spectral softening during the first outburst. Also, spectral modelling suggests that the first outburst is in the low/hard state throughout with a truncated disk whereas the thermal disk emission dominates during the second outburst. During the entire outburst, strong reflection signature (reflection fraction varies between ∼ 0.38 − 3.8) is observed in the simultaneous wideband (NICER-NuSTAR, XRT-NuSTAR, AstroSat) data due to the presence of a dynamically evolving corona. The NICER timing analysis shows Quasi-periodic Oscillation (QPO) signatures and the characteristic frequency increases (decreases) in the plateau (decline) phase with time during the first outburst. We understand that the reduction of the electron cooling timescale in the corona due to spectral softening and the resonance oscillation with the local dynamical timescale may explain the above behavior of the source during the outburst. Also, we propose a possible scenario of outburst triggering and the associated accretion geometry of the source.

Study of mass outflow rates from magnetized advective accretion disk around rotating black holes

“…Here, we choose α B = 0.005. Subsequently, using ṁ and a k for a given black hole, we 6.31 [79], [79], [80], [81], [81] GRO J1655−40 [82], [83], [84], [81], [ [85], [86], [87], [88], [89] GX 339−4 3.81 [94], [95], [96,97], [81], [81] IGR J17091−3624 10.6 − 12. 3 29.00 [109], [110], [111], [112], [112] MAXI J0637−430 † 0.79 [113], [114], [115], [115] [113], [114], [115], [115] V404 Cyg 15.21 [116], [117], [118], [119], [119] H 1743−322 7.44 [120], [121], [121], [122], [122] ⊠ Aneesha et al (2024)(under review).…”