Development of Components for Adaptive Optics Systems for Solar Telescopes

Botygina, N. N.; Emaleev, O. N.; Konyaev, P. A.; Kopylov, E. A.; Лукин, В. П.

doi:10.1134/s1024856018020057

“…LSVT is equipped with a mock-up of AO system. Using the experimental base of LSVT, methods and approaches have been developed for reconstructing wavefront distortions [Botygina et al, 2018;.…”

Section: Methods Of Measurements Of Wavefront Distortions Formed In T...mentioning

confidence: 99%

Turbulent parameters at different heights in the atmosphere. Shack–Hartmann wavefront sensor data

Shikhovtsev

¹

,

Kiselev

²

,

Kovadlo

³

et al. 2022

Solar-Terrestrial Physics

0

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The paper presents the results of studies of wavefront distortions at different heights in the atmosphere. We have used measurement wavefront data to determine optical turbulence parameters along the line of sight of the Large Solar Vacuum Telescope. Through cross-correlation analysis of differential motions of sunspots at spaced wavefront sensor subapertures, we determined turbulent parameters at different heights at the Large Solar Vacuum Telescope site. The differential motions of sunspots characterize the small-scale structure of turbulent phase distortions in the atmosphere. Synchronous temporal changes in the amplitude of these distortions at certain regions of the telescope aperture are conditioned by turbulent layers at different heights. We have estimated the contribution of optical turbulence to integral distortions at the telescope aperture for layers 0–0.6, 0.6–1.1, 1.1–1.7 km. The contribution of optical turbulence concentrated in a 1.7 km atmospheric layer to the wavefront distortions at the aperture telescope is shown to be ~43 %.

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“…БСВТ оснащен макетом системы АО. С использованием экспериментальной базы БСВТ развиты методы и подходы восстановления искажений волнового фронта [Botygina et al, 2018;Lavrinov, Lavrinova, 2019].…”

Section: используемый метод измерений искажений волнового фронта форм...unclassified

Turbulent parameters at different heights in the atmosphere. Shack–Hartmann wavefront sensor data

Shikhovtsev

¹

,

Kiselev

²

,

Kovadlo

³

et al. 2022

Solnechno-Zemnaya Fizika

0

View full text Add to dashboard Cite

The paper presents the results of studies of wavefront distortions at different heights in the atmosphere. We have used measurement wavefront data to determine optical turbulence parameters along the line of sight of the Large Solar Vacuum Telescope. Through cross-correlation analysis of differential motions of sunspots at spaced wavefront sensor subapertures, we determined turbulent parameters at different heights at the Large Solar Vacuum Telescope site. The differential motions of sunspots characterize the small-scale structure of turbulent phase distortions in the atmosphere. Synchronous temporal changes in the amplitude of these distortions at certain regions of the telescope aperture are conditioned by turbulent layers at different heights. We have estimated the contribution of optical turbulence to integral distortions at the telescope aperture for layers 0–0.6, 0.6–1.1, 1.1–1.7 km. The contribution of optical turbulence concentrated in a 1.7 km atmospheric layer to the wavefront distortions at the aperture telescope is shown to be ~43 %.

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“…When creating, adjusting, and testing adaptive optics systems used in astronomy and vision systems in a turbulent atmosphere [1][2][3][4][5][6], the problem of atmospheric turbulence emulation becomes relevant, for example, to stabilize the radiation image on the photoreceiving matrix of an optical system [7,8].…”

Section: Introductionmentioning

confidence: 99%

“…In the third module, the third optical beam is formed, generated by a laser (32), passes through a light filter (31), which sets its intensity, a pinhole diaphragm (30) and zooming optics (29), forming a collimated beam that passes through an adjustable diaphragm (28), which specifies the diameter of the emulated local inhomogeneity. When passing over the electric heating element (27), turbulent distortions of the wavefront are formed in the third beam, after which it enters the piezoceramic deflector (9), which sets the fluctuations in the beam tilt angle, and on the beam-splitting cube (10), the beam rotates 90 degrees and enters the beam-splitting cube (7), where it is aligned coaxially with the first (main) beam generated by the laser (1).…”

Section: Introductionmentioning

confidence: 99%

Emulation of atmospheric turbulence for image stabilization of laser radiation on the stand of adaptive optical system

Antoshkin

¹

,

Borzilov²,

Lavrinov³

et al. 2022

28th International Symposium on Atmospheric and Ocean Optics: Atmospheric Physics

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A description of the stand for an adaptive optics system operating in the mode of emulation of the slopes of the laser radiation wavefront on a turbulent path is given. The potential capabilities of the test bench involve setting the parameters of turbulent distortions characteristic of paths of various lengths, as well as using a piezceramic deflector of wavefront slopes as a source of emulated image distortions in the observation plane. The stand of the adaptive optics system makes it possible to stabilize the jitter of the optical radiation image in the plane of the receiving device with the adaptive correction circuit turned on and off under conditions of various system operation modes.

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Development of Components for Adaptive Optics Systems for Solar Telescopes

Cited by 13 publications

References 2 publications

Turbulent parameters at different heights in the atmosphere. Shack–Hartmann wavefront sensor data

Turbulent parameters at different heights in the atmosphere. Shack–Hartmann wavefront sensor data

Turbulent parameters at different heights in the atmosphere. Shack–Hartmann wavefront sensor data

Emulation of atmospheric turbulence for image stabilization of laser radiation on the stand of adaptive optical system

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