We analyzed UV spectra of twelve central stars of planetary nebula in the Large Magellanic Cloud. The observations were made with HST STIS in ultraviolet slitless spectroscopy mode, with gratings G140L and G230L. The spectra of the central stars were extracted from the 2D image. The high spatial resolution of HST allows separation of the nebular and stellar spectra. Further correction to the stellar extraction is provided by the nebular spectra themselves. The 1D spectra were then corrected for the galactic and LMC extinction. The stellar temperature and luminosities were derived by fitting the stellar continua, and constraining the fitting procedure by using the optical magnitudes derived from the optical HST data. The nebular contribution to the continuum were estimated via CLOUDY Some of the objects show P Cyg profile correspondent to the C IV 1548/1551 Å, Si IV 1394/1403 ÅÅ and N V 1239/1243 ÅÅ lines. We fit these lines using a line transfer code together with a genetic minimization algorithm. We report the obtained mass loss rates and terminal velocities. A comparison from our results with the ones obtained by other groups for central stars in Galactic planetary nebula is discussed.