WIND VARIABILITY IN THE LARGE MAGELLANIC CLOUD B[E] SUPERGIANT HD 34664

We present optical linear spectropolarimetry of the B[e] supergiant HD 34664. The polarization and position angle display significant spectr al features which correspond to the Halpha and Hbeta emission lines. W e use the line polarizations to separate the interstellar foreground p olarization from the intrinsic polarization of HD 34664. The intrinsic polarization is consistent with electron scattering in a circumstella r disk seen at high inclination and provides further and independent e vidence for the two-component wind model of the B[e] supergiants. We c ompare the polarization and spectrum of HD 34664 to observations publi shed in the literature. In our data the continuum polarization is by a factor of two larger and the Ha line-to-continuum ratio is by a facto r of at least four increased over previous observations. Since both th e polarization and the line intensity are measures of the electron den sity in the stellar wind, we suggest that the observed variations can be attributed to a rise in the stellar mass-loss rate.