Ejector and bipolar outflow of the radio galaxy M87

The superfine structure of the jet formation region in the radio galaxy M87 has been investigated. An accretion disk and high- and low-velocity jet and counterjet components have been identified. The high-velocity bipolar outflow is ejected from the central disk region, a nozzle 4 mpc in diameter, while the low-velocity one is ejected from a ring 60 mpc in diameter and 14 mpc in width. The low-velocity plasma flow is a hollow tube with a built-in helix. The observed helical structure of the high-velocity jet is determined by precession. The components of the structure, its disk and bipolar outflow, suggest solid-body rotation. Ring currents and aligned magnetic fields are generated in them under the action of an external magnetic field. The bipolar outflows are ejected coaxially but in opposite directions—along and opposite to the disk field. As a result, the jet flow accelerates, while the counterjet one decelerates. This causes the extent of the region of radiative cooling of the ejected relativistic electrons in the counterjet to decrease and maintains their “afterglow” at large distances in the jet. The high collimation of the rotating flows is determined by their interaction with the environment.