TURBULENT PARAMETERS AT DIFFERENT HEIGHTS IN THE ATMOSPHERE. SHACK–HARTMANN WAVEFRONT SENSOR DATA
Journal Title: Solar-Terrestrial Physics - Year 2022, Vol 8, Issue 2
Abstract
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 %.
Authors and Affiliations
Shikhovtsev A. Y. , Kiselev A. V. , Kovadlo P. G. , Kolobov D. Y. , Russkikh I. V. , Tomin V. E.
Keywords
Related Articles
- EP ID EP706570
- DOI 10.12737/stp-82202203
- Views 118
- Downloads 0
CORONAL JETS AS A CAUSE OF MICROWAVE NEGATIVE BURSTS
We have investigated the cause of three “isolated” negative radio bursts recorded one after another at several frequencies in the 1–17 GHz range at the Nobeyama Radio Observatory, Ussuriysk Astrophysical Observatory, and...
APPLYING THE METHOD OF MAXIMUM CONTRIBUTIONS TO THE MAGNETOGRAM INVERSION TECHNIQUE
Fundamentals of the spherical harmonic analysis (SHA) of the geomagnetic field were created by Gauss. They acquired the classical Chapman — Schmidt form in the first half of the XXth century. The SHA method was actively...
RELATION BETWEEN THE AREA OF POLAR CORONAL HOLES AND THE SOLAR WIND SPEED AT A MINIMUM BETWEEN SOLAR CYCLES 22 AND 23
We have used data from the space telescope SOHO/EIT and the spectrometer VEIS on the Wind spacecraft to compare the solar wind (SW) speed near Earth's orbit with changes in the area of polar coronal holes (CHs) on the Su...
COMPARING SIMULATED RESULTS OF FOLDED AND UNFOLDED LOG-PERIODIC ANTENNA USED FOR OBSERVING THE SUN
There are two antenna arrays located in Mingantu Spectral Radio Heliograph (MUSER). MUSER-I and MUSER-II cover the frequency band ranging from 0.4 to 2 GHz and from 2 to 15 GHz respectively. A third antenna array coverin...
COMPARISON BETWEEN PROBABILITY DENSITY FUNCTIONS OF VERTICAL ELECTRIC CURRENT IN SOLAR ACTIVE REGIONS BASED ON HMI/SDO AND SOT/HINODE DATA
Studying electric currents in solar active regions (AR) is an essential step in understanding solar activity in general and solar flares in particular. In this paper, we compare probability density functions of vertical...