its maxima (Figs. 3d, e, f). However, as the shock reaches its maximum value the thermal driving also recovers (Fig. 3g). The extra thermal driving plus the squeeze of the shock front as it shrinks, spews strong outflow (Fig. 3g). In Fig. 3f, we have indicated the shock location on the equatorial plane $r_s$, and the top of the shock front $r^T_s$. The position of the shock front can easily be identified from the clustering of the density contours connecting $r_s$ and $r^T_s$. From Figs. 3(a-h), it is clear that the mass outflow rate is significant when $r^T_s \gsim r_s$.

Due to shock transition, the post shock matter becomes hot and dense which would essentially be responsible to emit high energy radiation. At the critical viscosity, since the shock front exhibits regular oscillation, the inner part of the disc, CENBOL, also oscillates indicating the variation of photon flux emanating from the disc. Thus, a correlation between the variation of shock front and emitted radiation seem to be viable. Usually, the bremsstrahlung emission is estimated as, $$E_{Brem} = \int_{r_{1}}^{r_{2}} \rho^2 T^{1/2} r^2 dr,$$ where, $r_1$ and $r_2$ are the radii of interest within which radiation is being computed and $T$ is 