Abstract

It is known that atmospheric turbulence limits an angular resolution of ground-based astronomical imaging systems of the order of λ/r_o in size, where r_o is the coherent radius of the wavefront distorted by the atmosphere, typically values for visible spectral range Cλ= 0.55μm) under the good seeing conditions vary in 20 to 40 cm. Many designs of the ground-based telescopes provide using the system for adaptive (or active) correction of distortions of radiation wavefront of object observed. Here the need for modeling the operation of such systems arises.

© 1992 Optical Society of America