The massive interacting binary RY Scuti is an important representative of an active mass-transferring system that is changing before our eyes and which may be an example of the formation of a Wolf-Rayet star through tidal stripping . Utilizing new and previously published spectra , we present examples of how a number of illustrative absorption and emission features vary during the binary orbit . We identify spectral features associated with each component , calculate a new , double-lined spectroscopic binary orbit , and find masses of 7.1 \pm 1.2 ~ { } M _ { \odot } for the bright supergiant and 30.0 \pm 2.1 ~ { } M _ { \odot } for the hidden massive companion . Through tomographic reconstruction of the component spectra from the composite spectra , we confirm the O9.7 Ibpe spectral class of the bright supergiant and discover a B0.5 I spectrum associated with the hidden massive companion ; however , we suggest that the latter is actually the spectrum of the photosphere of the accretion torus immediately surrounding the massive companion . We describe the complex nature of the mass loss flows from the system in the context of recent hydrodynamical models for \beta Lyr , leading us to conclude RY Scuti has matter leaving the system in two ways : 1 ) a bipolar outflow from winds generated by the hidden massive companion , and 2 ) an outflow from the bright O9.7 Ibpe supergiant in the region near the L2 point to fill out a large , dense circumbinary disk . This circumbinary disk ( radius \approx 1 AU ) may feed the surrounding double-toroidal nebula ( radius \approx 2000 AU ) .