The emission line on the spectrum of the Wolf-Rayet star shows an exceptional abundance of the elements helium, nitrogen, carbon, and oxygen w hen compared to the spectrum of other stars. In this work, observation of WR 90 (HD 156385) was conducted using a low-resolution spectrograph at Bosscha Observatory. Determination of stellar parameters has been implemented using two different methods: The first method derives estimation of photosphere temperature and radius using the Black Body continuum model approximation, second method derives estimation of stellar temperature, radius, and luminosity using PoWR (The Postdam Wolf-Rayet) spectrum grid model. Furthermore, with the addition of the asymptotic terminal velocity derived from the Gaussian decomposition of the optical spectrum emission line and the P-Cygni profile analysis of the high-resolution IUE UV spectrum, the mass loss rate of the Wolf-Rayet star has been determined. The data used in both methods are low- and highresolution ultraviolet spectra retrieved from the IUE (International Ultraviolet Explorer) archival and optical spectrum of our observations. The obtained stellar parameters appear to have small differences when compared with previous work.