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tokens: ; Ghosh Chakrabarti 2018 ). So, Θ itself indicates (see Fig. 5 ), from its day-to-day time evolution, the arrival time lag, i.e. the size of the disc. It is shown recently by Ghosh et al. ( 2019 ) that the temporal evolution of RXTE /ASM soft and hard photon fluxes is, respectively, similar to that of disc and halo mass rates obtained from the TCAF-extracted RXTE /Proportional Counter Array (PCA) (2.5–25 keV) spectra. Also, during an outburst, the Comptonizing efficiency (CE) computed from ASM data behaves in a similar manner with the accretion rate ratio obtained from PCA data. According to TCAF, the Keplerian disc component is mainly responsible for the soft photon counts, whereas the halo component controls the hard photon counts. It is customary to assume soft and hard photons to represent multicolour blackbody distribution and power law, respectively (see Ghosh Chakrabarti 2018 ; Ghosh et al. 2019 ). Since TCAF is a general paradigm, it can be always utilized whether phenomenological descriptions such as power law plus blackbody fits the data already or not. Even if we have only ASM data, the knowledge of behaviour of the flows from TCAF enable us to choose Θ as the unique variable to classify the outbursts. Therefore, Θ is used for cross-correlation (CC) with individual fluxes, as the former represents relative change of one flux with respect to the other. So, the relative time lag between the hard flux and the soft flux of either photons or energy would be defined as (Ghosh Chakrabarti 2018 ), τ r > 0 implies that the disc radiation flux lags behind the halo radiation flux. Both evolve simultaneously if τ r = 0. Typical behaviour of Θ during a normal outburst is schematically shown in Fig. 4 . We wish to mention that while taking CCs, the direct hard flux versus soft flux correlation is not the proper quantity to discuss (see Fig. 6), because the hard flux does not depend on the soft flux alone. It also depends on the properties of the Compton cloud such as its size (CENBOL) and its optical depth. Furthermore, in an outburst, hard flux will always be seen increasing with the soft flux. So the lag between hard and soft, in general, would be seen to be zero. What is important is the rate at which two accreting masses change since these are guided by the viscosity in the halo and disc components. Since RXTE /ASM did not record X-ray data continuously from any particular source, there are gaps in the data, in particular, due to the annual solar constraints. We smoothed out the unevenness of the data interval by using a fortran code for interpolation. The fits files obtained from these daily light curves are used to produce CCs between Θ and two fluxes using crosscor task of heasoft/xronos package in order to obtain the time lags estimated from Θ. 3 RESULTS We present the photon energy fluxes, Θ-behaviour, their CCs, and most importantly, the hysteresis property of the standard Keplerian disc for showing difference in temporal and spectral