2000ApJ...531.1003R

The circumstellar environment in the system changes in cycles of hundreds of days. The length of the cycles is variable. These cycles may be part of a ``super'' 4000 day cycle.

The equivalent widths of the difference Hα and He I λ6678 lines are modulated with the orbital period of 6.696 days. The corresponding phase diagrams indicate a great deal of scatter, but the modulation is quite conspicuous when long data strings are used. The pattern of the phase diagram suggests a permanent presence of the emission in Hα, He I λ6678, and Si II λ6371 lines.

The radial velocities of the Hα emission peak follow an S-wave. The resulting velocity map shows that the source of the single-peaked emission lies close to the L1 point, roughly between the primary and L1 point.

Doppler tomograms constructed for Hα observed and difference profiles show that the emission comes from a region of low velocity, a gas stream, and an accretion disk. The Hβ emission arises from a region that is cospatial with the Hα source. The Doppler tomograms for He I λ6678 and Si II λ6371 lines suggest that emission in this gas also originates from a locus of a disk around the primary star.

The model based on the equivalent widths of the difference profiles, the trailed spectrograms, and Doppler tomograms of the Hα, He I λ6678, Si II λ6371, and Hβ lines suggests that the main source of the Hα emission is about halfway between the stars at a distance of 0.49a from the primary star, and that the He I and Si II emission sources arise from an accretion disk centered on the primary star.