We show the isolated convection bay followed after a classic substorm to compare and contrast their signatures. Both events, caused by the southward IMF episodes, displayed the enhanced convection, comparable Dst decreases and auroral zone Pi2 pulsations. Unlike the substorm event, the signatures of energy loading/unloading and near-Earth reconnection (lobe field changes, poleward auroral expansion, SCW growth, strong injection to 6.6 Re) were virtually absent during the convection bay. We emphasize the auroral dynamics, which was basically organized by multiple auroral streamers which start sporadically at the poleward boundary of wide double oval, propagate equatorward (in 3-8 min) and end with a long-duration bright spot in the equatorward oval. Streamers are closely associated with the plasma sheet BBFs and short, narrow and soft injections to 6.6 Re. We argue that the 'pressure crisis' in the tail plasma sheet was significantly reduced during the convection bay and that Earthward transport by sporadic narrow (similar to3 Re wide) plasma jets (plasma bubbles) from distant reconnection regions to the inner magnetosphere was efficient enough to avoid the energy loading and resulting substorm instability in the tail.