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We present an analysis of the potential follow-up polarimetry microlensingobservation to study the stellar atmospheres of the distant stars. First, weproduce synthetic microlensing events using the Galactic model, stellarpopulation, and interstellar dust toward the Galactic Bulge. We simulate thepolarization microlensing light curves and pass them through the instrumentspecifications of FOcal Reducer and low dispersion Spectrograph (FORS2)polarimeter at Very Large Telescope (VLT), and then analyze them. We find thatthe accuracy of the VLT telescope lets us constrain the atmosphere of cool RGBstars. Assuming detection of about $3000$ microlensing events per year by theOGLE telescope, we expect to detect almost $20,~10,~8, $ and $5$ ofpolarization microlensig events for the four different criteria of being threeconsecutive polarimetry data points above the baseline with $1\sigma$,$2\sigma$, $3\sigma$, and $4\sigma$, respectively in the polarimetry lightcurves. We generalize the covariance matrix formulation and present thecombination of polarimetry and photometry information that leads us to measurethe scattering optical depth of the atmosphere and the inner radius of thestellar envelope of red giant stars. These two parameters could determine thedust opacity of the atmosphere of cool RGB source stars and the radius wheredust can be formed.

Measuring the stellar atmosphere parameters using follow-up polarimetry microlensing observations