DYNAMICALLY DETERMINED MASSES FROM HIGH MASS BINARY SYSTEMS ARE THE OBSERVATIONAL CONSTRAINTS FOR STELLAR INTERIOR MODELS. THESE MODELS WITH THE INCLUSION OF ANGULAR MOMENTUM AND METALLICITY-DEPENDENT MASS LOSS PREDICT THAT MASSIVE STARS AT LOW Z WILL LOSE LESS MASS AND ANGULAR MOMENTUM AS THEY EVOLVE. BOTH THE COLLAPSAR MODEL FOR GAMMA RAY BURSTS AND THE MERGING 30 SOLAR MASS BH-BH SYSTEMS DISCOVERED THROUGH GRAVITATIONAL WAVES DEPEND UPON THIS PREDICTION TO FORM THE NECESSARY EVOLVED HIGH MASS HIGH ANGULAR MOMENTUM PROGENITOR SYSTEMS. THE STRUVE-SAHADE EFFECT ALONG WITH OTHER PHASE DEPENDENT SPECTRAL VARIABILITY CASTS DOUBT ON OUR ABILITY TO ACCURATELY DETERMINE THE MASSES (AND ROTATIONAL VELOCITIES) FROM THESE MASSIVE SYSTEMS. THE S-S EFFECT IS DESCRIBED AS THE APPARENT STRENGTHENING OF A STAR S SPECTRUM AS IT APPROACHES AND WEAKENING AS IT RECEDES. DESPITE BEING WELL-KNOWN FOR OVER 100 YEARS AND ITS PROLIFIC NATURE AMONG MASSIVE BINARIES WE STILL DO NOT UNDERSTAND THE UNDERLYING CONDITIONS BEHIND IT OR THE IMPACT THAT IT MAY HAVE ON OUR DERIVED ORBITAL PARAMETERS. COMPETING THEORETICAL MODELS OF THE S-S EFFECT BY GIES ET AL. (1997) AND GAYLEY ET AL. (2007) PROVIDE CLEAR OBSERVATIONAL DIAGNOSTICS THAT REQUIRE HIGH-RESOLUTION SPECTROSCOPY WITH COMPLETE PHASE COVERAGE OF MULTIPLE BINARY SYSTEMS. THE GAYLEY ET AL. (2007) MODEL SPECIFICALLY REQUIRES A LARGE RANGE IN ABSORPTION LINE FORMATION DEPTH AS IT PREDICTS THAT THE EFFECT WOULD NOT AFFECT LINES FORMED DEEP IN THE PHOTOSPHERE. IN THE FINAL OPERATIONAL YEARS OF THE INTERNATIONAL ULTRAVIOLET EXPLORER EFFORTS WERE MADE TO OBTAIN COMPLETE PHASE COVERAGE OF EVERY HIGH MASS BINARY OBSERVABLE BY THE SHORT WAVELENGTH PRIME (SWP) INSTRUMENT RESULTING IN OVER 600 SPECTRA OF 23 SB2 O-TYPE SYSTEMS. THESE ULTRAVIOLET SPECTRA FORMED AT THE PLANCK PEAK OF THESE HOT STARS HAVE HUNDREDS OF ABSORPTION FEATURES (FE V FE IV HE II C III SI IV O IV O V ETC.) WITH A LARGE RANGE OF IONIZATION AND EXCITATION POTENTIALS. WE PROPOSE TO ANALYZE THESE SYSTEMS USING THE DIAGNOSTICS LAID OUT BY THE COMPETING THEORETICAL MECHANISMS. WE ALSO WILL DETERMINE WHAT IMPACT IF ANY THE SPECTRAL VARIABILITY PRESENT HAS ON THE DERIVED MASSES. AS A TEST OF OUR METHODS WE PRESENT RESULTS FOR THE O-TYPE BINARY HD159176 THAT LARGELY SUPPORT THE GAYLEY EL AL. (2007) MODEL.