  If a massive star has lost significant mass during its red-supergiant stage,
it would return to blue region in the HR diagram and spend a part of the
core-He burning stage as a blue supergiant having a luminosity to mass ratio
(L/M) considerably larger than about 10^4 (in solar units); the duration
depends on the degree of internal mixing and on the metallicity. Then, various
stellar pulsations are excited by enhanced \kappa-mechanism and strange mode
instability. Assuming these pulsations to be responsible for (at least some of)
the quasi-periodic light and radial-velocity variations in \alpha Cygni
variables including luminous blue variables (LBVs; or S Dor variables), we can
predict masses and surface compositions for these variables, and compare them
with observed ones to constrain the evolutionary models. We discuss radial
pulsations excited in evolutionary models of an initial mass of 40 M_\odot with
solar metallicity of Z=0.014, and compare them to micro-variations in the two
Galactic LBVs, HR Car and HD 160529. We have found that these stars should has
lost more than half of the initial mass and their surface CNO abundances should
be significantly modified from the original ones showing partial H-burning
products.
