2023PASJ...75..677I

The ejection mechanism of transient relativistic jets from black hole binaries is studied. Based on observations of the limit-cycle behaviors of the superluminal jet source GRS 1915+105, we infer that transient jet ejections could happen just after the slim disk emerging from the standard disk at some distance runs over the standard disk and reaches the vicinity of the central black hole. The standard disk releases about half of the gravitational energy in the course of the accretion, but the released radiative energy could be absorbed by the optically thick slim disk covering the standard disk in this situation. Then, since the inward motion of the slim disk is much faster than that of the standard disk, a quantity of energy released by an amount of gas in the standard disk is received by the much smaller amount of gas in the slim disk. As a result, the energy per mass received by the slim disk is expected to be greatly amplified and is estimated to become highly relativistic. Since the energy is much larger than the gravitational energy, the height of the slim disk could increase significantly. Hence, the innermost part of the slim disk from which almost all the angular momentum has been transferred outward could have a much larger height than the black hole size, so they could collide with one another around the central axis of the disk, turning to an outward flow along the axis normal to the disk plane. The flow in this direction can be approximated to be that through the de Laval nozzle and could become supersonic near the distance where the flow has the smallest cross-section.