Cartoon schematic showing how the emission may vary with Eddington ratio. Left: sources with relatively lower Eddington ratios (few ×10⁻³), there is sufficient radiation pressure to launch line driven winds, but not so much that the winds become over-ionised, so more warm absorbers are detected. Middle: sources with intermediate Eddington ratios, (few ×10⁻²) some winds will become over-ionised and their velocities will not exceed the escape velocity and will fail, but will remain somewhat bound to the system, creating patchy partial covering absorbers. Right: sources accreting at 0.1 − 1 Eddington, high radiation pressure results in too many ionising photons and the wind is destroyed, remaining tightly bound to the system and forming the warm corona.