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Methods for reconstructing the high-altitude profiles of optical turbulence from the observations of single bright stars
The techniques for reconstructing the altitude profiles of the optical turbulence (OT) intensity using the data on the distortion of the front of a light wave passing through the atmosphere are considered and implemented. They involve an observation of single bright stars (0m–2m) with a small 250–300 mm telescope equipped with a Shack-Hartmann wavefront sensor. The methods of reconstructing the altitude OT profile based on the Kolmogorov and Von-Karman theory are considered. The advantages and disadvantages of using the weight functions for scintillations in paired subapertures and differential slopes are discussed separately. It is concluded that there are serious disadvantages in the methods using scintillations. The efficiency of different techniques is demonstrated using the real data obtained at the stationary astroclimatic monitors in the Moscow Oblast and the Altai Republic.