Results of spectroscopy of an unusual symbiotic variable star MWC 560 are presented, obtained from autumn 1990 to spring 1993. The high velocity absorption line profiles suggest that they originate in a jet, directed closely to the line of sight. A fast variability of the absorption line profiles on a time scale of ⪉3 hours has been detected. Evidence of an opposite (second) jet has been found. Estimates of the orbital inclination angle (i ≍ 10°) and the jet parameters have been made. The authors suppose that both the wind and jets are accelerated in the magnetic field of the white dwarf, which accretes the gas from the giant wind as a propeller. The gas flows in accretion disk and is expelled from that by the rotating magnetic field. A sectorial structure of the outflow (jets) is formed. The different states of MWC 560 may correspond to different propeller regimes: a hard propeller with a gas velocity outflow a few thousands of km/s and a soft propeller with a few hundred km/s.