摘要：We examine over 160 archival Hα spectra from the Ritter Observatory for the interacting binary βLyr obtainedbetween 1996 and 2000. The emission is characteristically double-peaked, but asymmetric, and with an absorptionfeature that is persistently blueshifted. Using a set of simplifying assumptions, phase varying emission line profilesare calculated for Hα formed entirely in a Keplerian disk, and separately for the line formed entirely from an off-center bipolar flow. However, a dynamic spectrum of the data indicates that the blueshifted feature is not alwayspresent, and the data are even suggestive of a drift of the feature in velocity shift. We explore whether acircumbinary envelope, hot spot on the accretion disk, or accretion stream could explain the observations. Whilenone are satisfactory, an accretion stream explanation is somewhat promising.
