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By conducting three-dimensional (3D) hydrodynamical simulations we find thatjets that a main sequence companion launches as it orbits inside the windacceleration zone of an asymptotic giant branch (AGB) star can efficientlyremove mass from that zone. We assume that during the intensive wind phase alarge fraction of the gas in the acceleration zone does not reach the escapevelocity. Therefore, in the numerical simulations we blow the wind with avelocity just below the escape velocity. We assume that a main sequencecompanion accretes mass from the slow wind via an accretion disk, and launchestwo opposite jets perpendicular to the equatorial plane. This novel flowinteraction shows that by launching jets a companion outside a giant star, butclose enough to be in the acceleration zone of a slow intensive wind, canenhance the mass loss rate from the giant by ejecting some gas that wouldotherwise fall back onto the giant star. The jets are bent inside the windacceleration zone and eject mass in a belt on the two sides of the equatorialplane. The jet-wind interaction contains instabilities that mix shocked jets'gas with the wind, leading to energy transfer from the jets to the wind. Aswell, our new simulations add to the rich variety of jet-induced outflowmorphologies from evolved stars.

A companion star launching jets in the wind acceleration zone of a giant star