Luminous Blue Variables are evolutionary massive stars. Their most distinct characteristic is irregular light variations at different timescales. Up to now these models for explanting the phenomenon are not successful. In fact we even don’t know basic physic parameters of some LBVs. Combine the spectra of IUE with photometric data Models for the continua of luminous blue variables in minimum and maximum states are calculated. We found that the mass-loss increase by itself cannot account for the decrease of the effective temperature. The increase of the mass loss rate causes only a comparatively small change in the radius of continuum formation. The observed light variations could be induced from deeper stellar envelope. In addition, via fitted the continua of LBVs we may determine the properties of the wind. We found that the velocity gradient of winds of LBVs is stepper in the minimum phase. The exponent (β) of the wind velocity equals 0.5 and more than 1 in the minimum and maximum state, respectively. We determine also the geometry of the wind. A spherical wind may reproduce the observed continua. These observed polarizations, which are variable in both strength and position angle, could hint that the localized density enhancements, or `clumps' could be exist in the base of the wind. For R 110 and R 127 both show two peaks in the continua. We consider that the continua of both stars could be “contaminated” by optical companion. All LBVs display evidence for intrinsic uniformity.
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