Abstract
ABSTRACT Spectroscopic, time-resolved observations of the accretion disk in the long-period Algol system RY Gem during eclipse are presented. It is shown that the disk is non-Keplerian and has asymmetries between the leading and trailing sides of the accretion disk similar to those seen in the transient disks of the short-period Algol systems. There is about 50 km/s difference in the rotational velocity between the leading and trailing sides of the disk. The rotational velocity of the leading side appears to be sub-Keplerian. The linewidths on the trailing side are larger than expected for a rotationally broadened line and they do not vary during eclipse. Similar linewidths are seen from a portion of the leading side. Taken together this suggests the presence of turbulence like that proposed to exist in the transient disk systems. At least a portion of the gas stream from the secondary star strikes the trailing side of the accreting star. Apparently this collision and the subsequent interaction of the gas circling the star with the incoming stream produce a structure very similar to a transient disk.
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