| Abstract: We conduct a comprehensive spectro-temporal analysis in more than twenty BH-XRBs such as XTE J1859+226, 4U 1543−47, H1743−322, GX 339-4, XTE J1550−564, XTE J1752−223, XTE J1650−500, Swift J1753.5−0127, XTE J1748−288, GRO J1655−40, Swift J1727.8-1613, MAXI J1535-571, MAXI J1820+070, MAXI J1348-630, Swift J1658.2−4242, MAXI J1803-298 source, V404 Cyg, V4641 Sgr, Cyg X-3, GRS 1915+105, GRS 1758–258 and 1E 1740.7-2942 using AstroSat, RXTE, and HXMT observations (quasi-) simultaneous with radio observations. In the majority of these sources, we observe an increase in X-ray flux preceding the radio flares. Additionally, the presence of type-A/B QPOs (and occasionally the disappearance of QPOs) is observed during the radio flares, suggesting a connection between these QPOs and jet launching. Further, we observe a positive correlation between the QPO rms (1% - 15%) and normalized Comptonized flux (Fnth ~ 0.02-0.93) across all QPO types and inclination angles. In case of high inclination sources, type-B QPOs exhibit both positive and negative lags, whereas in low inclination sources, they exhibit only positive lag. On the other hand, type-A QPOs always exhibit a negative lag, regardless of the inclination. This implies a possible evolution of coronal geometry from radial to vertically elongated before jet ejections. During hard to softer state transitions, the jet velocities are constrained as ~0.3-0.8 c, and a positive correlation is observed between X-ray and radio fluxes. This suggests that the jet activity is possibly powered by an accretion process. |
