Identifying low-amplitude pulsating stars through microlensing observations

One possibility for detecting low-amplitude pulsational variations is through gravitational microlensing. During a microlensing event, the temporary brightness increase leads to improvement in signal-to-noise ratio, and thereby better detectability of signatures light curves. We explore this under two primary considerations. The first when standard point-source point-lens approximation applies. In scenario, dividing observed curve by best-fitted model residuals that result features with improved uncertainties. second transit events (single lens) or caustic crossing (binary lens). breaks down, relative simple display more complex behavior. employ Monte-Carlo simulation pulsating variables toward Galactic bulge surveys OGLE KMTNet. demonstrate efficiency intrinsic amplitudes $<0.25$ mag during single binary events, at differences $\chi^{2}$ $\Delta \chi^{2} >350$, $\sim 50-60\%$. maximum occurs periods $P \simeq 0.1-0.3$ days. also study high-magnification non-radially stars (NRPs) could be misinterpreted as planetary events. conclude small asymmetric around lightcurve peaks due stellar pulsations misdiagnosed (or passing close to)