The accretion stream, which follows a free-falling, ``ballistic'' trajectory from the inner Lagrangian point to the disk edge in non-magnetic cataclysmic variables (CVs), is presumed to be channeled over field lines and directly onto the magnetic pole(s) of the white dwarf (WD) primary star in high field strength magnetic CVs. We use Doppler tomograms of 3 high field CVs (V1309 Ori, B 60 MG; V884 Her, B 120 MG; AR UMa, B 230 MG) to explore the influence of the magnetic field on the accretion flow in high field CVs. Tomography can be used to constrain the mass ratios and orbital velocities in these systems. Surprisingly, tomograms of AR UMa suggest that even its very strong magnetic field does not control accretion all the way from the L1 point to the WD.
Annapolis Workshop on Magnetic Cataclysmic Variables
- Pub Date:
- V1309 ORI;
- V884 HER;
- AR UMA