You have requested a machine translation of selected content from our databases. This functionality is provided solely for your convenience and is in no way intended to replace human translation. Neither SPIE nor the owners and publishers of the content make, and they explicitly disclaim, any express or implied representations or warranties of any kind, including, without limitation, representations and warranties as to the functionality of the translation feature or the accuracy or completeness of the translations.
Translations are not retained in our system. Your use of this feature and the translations is subject to all use restrictions contained in the Terms and Conditions of Use of the SPIE website.
15 December 1995Atmospheric scintillations for measuring remote wavefronts
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
"Atmospheric scintillations for measuring remote wavefronts", Proc. SPIE 2580, Optics in Atmospheric Propagation and Adaptive Systems, (15 December 1995); https://doi.org/10.1117/12.228480
The alert did not successfully save. Please try again later.
Erez N. Ribak, "Atmospheric scintillations for measuring remote wave fronts," Proc. SPIE 2580, Optics in Atmospheric Propagation and Adaptive Systems, (15 December 1995); https://doi.org/10.1117/12.228480