Rohan Raha IISc, Koushik Chatterjee Maryland, Banibrata Mukhopadhyay IISc

Using high-resolution general relativistic magnetohydrodynamic (GRMHD) simulations, we investigate accretion flows around spinning black holes and identify three distinct accretion states. Our results naturally explain some of the complex phenomenology observed across the black hole mass spectrum. The magnetically arrested disk (MAD) state, characterized by strong magnetic fields (plasma-$\beta << 1$), exhibits powerful jets (of power $\sim10^{39}$ erg s$^{-1}$), highly variable accretion, and significant sub-Keplerian motion. On the other hand, weakly magnetized disks (plasma-$\beta >> 1$), known as the standard and normal evolution (SANE) state, show steady accretion with primarily thermal winds. An intermediate state bridges the gap between MAD and SANE regimes, with moderate magnetic support (plasma-$\beta \sim 1$) producing mixed outflow morphologies and complex variability. This unified framework explains the extreme variability of GRS 1915+105, the steady jets of Cyg X-1, and the unusually high luminosities (even super-Eddington based on stellar mass black hole) of HLX-1 without requiring super-Eddington mass accretion rates. Our simulations reveal a hierarchy of timescales that explain the rich variety of variability patterns, with magnetic processes driving transitions between states. Comparing two with three dimensional simulations demonstrates that while quantitative details differ, the qualitative features distinguishing different accretion states remain robust. The outflow power and variability follow a fundamental scaling relation with mass determined by the magnetic field configuration, demonstrating how similar accretion physics operates from stellar-mass X-ray binaries (XRBs) to intermediate mass black hole sources. This could be extrapolated further to supermassive black holes.