The 2018 outburst of MAXI J1820+070 as seen by Insight-HXMT

Abstract

We present an analysis of the whole 2018 outburst of the black hole X-ray binary MAXI J1820+070 with Insight-HXMT data. We focus our study on the temporal evolution of the parameters of the source. We employ two different models to fit the disk's thermal spectrum: the Newtonian model DISKBB and the relativistic model NKBB. These two models provide different pictures of the source in the soft state. With DISKBB, we find that the inner edge of the disk is close to the innermost stable circular orbit of a fast-rotating black hole and the corona changes geometry from the hard to the soft state. With NKBB, we find that the disk is truncated in the soft state and that the coronal geometry does not change significantly during the whole outburst. However, the model with NKBB can predict an untruncated disk around a fast-rotating black hole if we assume that the disk inclination angle is around $30^{\circ }$ (instead of $\sim 60^{\circ }$, which is the inclination angle of the jet and is usually adopted as the disk inclination angle in the literature) and we employ a high-density reflection model. In such a case, we measure a high value of the black hole spin parameter with observations in the soft state, in agreement with the high spin value found from the analysis of the reflection features and in disagreement with the low spin value found by previous continuum-fitting method measurements with the disk inclination angle set to the value of the jet inclination angle.

14 pages, 8 figures. v2: refereed version

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• Variable QPO lags and reduced coherence between the disc and corona in MAXI J1820+070
• Measuring black hole spins with x-ray reflection spectroscopy: A GRMHD outlook
• Possible Coronal Geometry in the Hard and Soft State of Black Hole X-ray Binaries from MONK Simulations
• Accretion Geometry of Black Hole X-ray Binaries: Insights from X-ray Observations
• NICER Spectral and Timing Analysis of 4U 1630$-$47 and its Heartbeat State