2021ApJ...914..111G

We compute successfully the launching of two magnetic winds from two circumbinary disks formed after a common envelope event. The launching is produced by the increase of magnetic pressure due to the collapse of the disks. The collapse is due to internal torques produced by a weak poloidal magnetic field. The first wind can be described as a wide jet, with an average mass-loss rate of ∼1.3 x 10^–7 M_☉ yr^–1 and a maximum radial velocity of ∼230 km s^–1. The outflow has a half-opening angle of ∼20°. Narrow jets are also formed intermittently with velocities up to 3000 km s^–1, with mass-loss rates of ∼6 x 10^–12 M_☉ yr^–1 during short periods of time. The second wind can be described as a wide X-wind, with an average mass-loss rate of ∼1.68 x 10^–7 M_☉ yr^–1 and a velocity of ∼30 km s^–1. A narrow jet is also formed with a velocity of 250 km s^–1 and a mass-loss rate of ∼10^–12 M_☉ yr^–1. The computed jets are used to provide inflow boundary conditions for simulations of proto-planetary nebulae. The wide jet evolves into a molecular collimated outflow within a few astronomical units, producing proto-planetary nebulae with bipolar, elongated shapes, whose kinetic energies reach ∼4 x 10⁴⁵ erg at 1000 yr. Similarities with observed features in W43A, OH 231.8+4.2, and Hen 3-1475 are discussed. The computed wide X-wind produces proto-planetary nebulae with slower expansion velocities, bipolar and elliptical shapes, and possible starfish-type and quadrupolar morphology.