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T. Koupelis (Univ. of Wisconsin - Marathon), J. M. Hollis (NASA/GSFC)
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 UV regimes, helical structure seen in UV emission, and suggests a parcel structure with its UV emission forming a low density sheath surrounding its radio region which is more dense 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 of ~ 4.6 x 109 G if a sub dwarf of radius 7 x 109 cm or, alternatively, ~ 2.3 x 1011 G if a white dwarf of radius 109 cm. The implications of such a model are discussed. J. M. H. received support from NASA RTOP 344-02-03-01 and T. K. received support from NSF AST-9318745.
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