As part of a broad study of stellar winds in different galaxies, to establish observational constraints on the influence of metallicity on the mass loss process, we investigate the winds of planetary nebula (PN) nuclei in the Large Magellanic Cloud. Theoretically, the radiation pressure mechanism implies a strong dependence of the wind acceleration on the element abundances. Observationally, model predictions have been tested using Pop. I stars in the Magellanic Clouds (Puls et al. 1996, A&A, 305, 171) and massive stars in the nearby galaxies M31, M33 and NGC 6822 (Bianchi et al. 1996, AJ, 111, 2303; Bianchi et al. 1996, in prep.). We now extend this investigation to low luminosity, evolved objects.