BASIC PHYSICAL MECHANISMS DURING MAXI J1535-571 OUTBURST EVOLUTION

MAXI J1535-571 outburst on September 02, 2017. The accretion-flow constituents, Keplerian and subKeplerian flows, contain optically thick and optically thin plasma that explain the nature of X-ray emission. The accretion flow geometry of MAXI J1535-571 and the mechanisms responsible for the physical phenomena observed in accretion flows are still debated. In this study, MAXI/GSC, NuSTAR, and Swift/BAT data were reanalyzed and fitted using HEASoft v6.28, the pipeline product software for each X-ray detector, XSPEC v12.10.1f, and a combination of accretion flow models. Acceptable statistically fitted MAXI J1535-571 X-ray spectra were obtained. Accretion flow parameters were correlated, and the correlation is statistically significant. Mass accretion rates are intrinsic properties of the accretion flow, and their interaction at varying distances and proportions created similar physical features in other accretion flow parameters. The interaction of components of the accretion flow and their mass accretion rates is responsible for the production of propagating oscillatory shock waves (Quasi-periodic oscillations; QPOs), a decrease in accretion rate ratio (ARR), a delay in spectral transition period, and explains the dynamics/geometry of the accretion flow, and the outburst characteristics of MAXI J1535-571.