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In the last decade the quality and the amount of observational asteroseismicdata that has been made available by space based missions had a tremendousupgrowth. The determination of asteroseismic parameters to estimate thefundamental physical processes occurring in stars' interiors, can be done todayin a way that has never been possible before. In this work we propose tocompute the seismic observable $\beta$, which is a proxy of the phase shift ofthe acoustic modes propagating in the envelope of the Sun-like stars. Thisseismic parameter $\beta$ can be used to identify rapid variation regionsusually known as glitches. We show that a small variation in the structure,smaller than 1% in the sound speed, produces a glitch in the acoustic potentialthat could explain the oscillatory character of $\beta$. This method allows usto determine the location and the thickness of the glitch with precision. Weapplied this idea to the Sun-like star $\alpha$ Centauri A and found a glitchlocated at approximately $0.94\,R$ (1400 s) and with a thickness of 0.2% of thestars' radius. This is fully consistent with the data and also validates otherseismic tests.

Local perturbations of the upper layers of a Sun-like star: the impact on the acoustic oscillation spectrum