In this paper, wide-field adaptive optics systems for ground-based solar telescopes are discussed. The features of constructing adaptive optics systems based on layer- and object-oriented approaches are considered. It is shown that the optimal adaptive optics system for the Large Solar Vacuum Telescope (LSVT) should be created on the basis of optical conjugation of deformable mirrors with turbulent layers of the atmosphere, the system for determining wavefront aberrations should be based on the use of a set of a narrow field of view sensors conjugated with telescope aperture, as well as a multi-directional wavefront sensor for turbulence tomography, designed on the basis of an object-oriented approach (measurements of wavefront aberrations in different directions). The schemes of pupil imagers that provide optical conjugation of the LSVT wavefront sensor with heights of 3 km as well as the upper atmospheric levels are considered. Direct optical conjugation of the Shack-Hartmann sensor with a turbulent layer is limited by a height of about 3 km (due to significant vignetting).
The quality of astronomical observations is strongly related to the quality properties of the atmosphere. The studies of the atmosphere above observing sites are important for observation planning, instrument optimization, adaptive optics development. The high-altitude distributions of wind speed over the 6-meters Big Telescope Alt-Azimuthal of Special Astrophysical Observatory of Russian Academy Science for astronomical site characterization and the development of adaptive optics techniques are study. The data used from the NCEP/NCAR and ERA-Interium reanalysis, which is widely acknowledged as being reliable. Seasonal behaviors (mean, median, quantiles) of vertical distributions of wind speed are presented. Statistical analyses of the 200-mbar wind speed used as useful parameter for ranking astronomical sites in term of their suitability for adaptive optics is performed. The long-time trend of V200 is presented.
The work discusses the optical turbulence structure and dynamics at the Baykal Astrophysical Observatory (BAO) site. The characteristics of the optical turbulence including Fried radius, isoplanatic angle are analyzed. Estimates of the variations of the height profiles of the air refraction index turbulent fluctuations at the Baykal Astrophysical Observatory are given. Using the mean height profile of the structure characteristic of the air refraction index turbulent fluctuations, diurnal variations of the Fried radius at the BAO site are estimated.
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