Stellar scintillations provide statistical information about the higher atmosphere (7 - 12 km). Since each realization of scintillation is the Fresnel diffraction off high altitude turbulence, it can be inverted separately. Sensors for adaptive optics integrate the wave front error over all layers of turbulence. They measure scintillation for calibration. But this discarded information yields the high wave fronts. Separate correction for low and/or high turbulence widens the repaired field of view. The method requires that the reference star is bright and small, that the middle turbulence (2 - 7 km) is negligible, and that the sensor has good spatio-temporal resolution. Simulations show that the turbulence can be retrieved, with lowest and highest frequencies lost first.
Erez N. Ribak, Erez N. Ribak,
"Atmospheric scintillations for measuring remote wavefronts", Proc. SPIE 2580, Optics in Atmospheric Propagation and Adaptive Systems, (15 December 1995); doi: 10.1117/12.228480; https://doi.org/10.1117/12.228480