Flux distribution in the Algol binary system RW Persei

IUE low-dispersion spectra and optical TIS scans of the Algol-type binary system RW Persei show that the primary has a spectrral type of B9.6 and that it is a Be star. The cooler component has a spectral type that is less accurately determined to as K2 III-IV, and it is probably a star of very low mass. The system is heavily reddened, with an E(B-V) color excess of 0.40 + or - 0.05 mag. The present results suggest that the hotter component is actually an opticaly thick accretion disk. The expected W Serpentis-type emission lines are not found in the UV spectrum near mideclipse, although two very broad emissions and several weaker ones seem to be present.