R Aquarii jet: Lorentz force-driven parcel model

The R Aqr symbiotic star system shows directed ow in the form of individual jet parcels. A parcel model for the R Aqr jet is developed that depends upon the strong stellar magnetic field of the rotating hot companion in the system. The model accounts for observed velocities seen in both the radio and ultraviolet regimes and for helical structure seen in ultraviolet emission, and suggests a parcel structure with its ultraviolet emission forming a low-density sheath surrounding its radio region, which is denser by a factor of similar to 30. The model predicts that the rotation of the hot companion is similar to 18 yr, which is a significant fraction of the similar to 44 yr orbital period, and frozen magnetic field flux conservation suggests that the hot companion has a surface held between 9 x 10(7) and 4.6 x 10(9) G if it is a subdwarf of radius 7 x 10(9) cm, or, alternatively, between 4.4 x 10(9) and 2.3 x 10(11) G if it is a white dwarf of radius 10(9) cm. The implications of such a model are discussed.