Continuing the theme of the previous two papers, the link between the stellar components of a highly-magnetic CV is considered with emphasis on the current strongest-field example, ar. Progress toward a detailed understanding of this binary includes an accurate orbital ephemeris and the derivation of a system geometry that implies two accretion streams which arc high above and below the orbital plane. From our vantage point, the dynamically-favored pole is likely hidden from view over the entire orbit. The idea of magnetic ``throttling'' of the mass flow through l1 has some credence for very high-field systems, but it appears that too little gas can accumulate in the magnetosphere to be responsible for the episodic accretion behavior exhibited by ar.
Annapolis Workshop on Magnetic Cataclysmic Variables
- Pub Date:
- AR UMA