SIMBAD references

The R Aqr symbiotic star system shows directed flow 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 ∼30. The model predicts that the rotation of the hot companion is ∼18 yr, which is a significant fraction of the ∼44 yr orbital period, and frozen magnetic field flux conservation suggests that the hot companion has a surface field between 9x10⁷ and 4.6x10⁹ G if it is a subdwarf of radius 7x10⁹ cm, or, alternatively, between 4.4x10⁹ and 2.3x10¹¹ G if it is a white dwarf of radius 10⁹ cm. The implications of such a model are discussed.