Journal of Physical Studies 23(1), Article 1902 [6 pages] (2019) DOI: https://doi.org/10.30970/jps.23.1902 STUDIES OF ACTIVE FORMATIONS IN THE PHOTOSPHERE WITH A SOLAR TELESCOPE ATsU-26 S. M. Chornogor1, M. V. Karpov2, O. V. Andrienko2, Yu. S. Ivanov2, L. I. Karpova2 1Main Astronomical Observatory NAS of Ukraine, 27, Akademik Zabolotny St., Kyiv, UA--03143, Ukraine 2International Center for Astronomical and Medico-Ecological Research NAS of Ukraine 27, Akademik Zabolotny St., Kyiv, UA--03143, Ukraine e-mail: karpov@mao.kiev.ua

The paper describes the capabilities and the current state of the horizontal solar telescope AZU-26, as well as considers a control hardware-software complex targeting and guiding the telescope. Studies of flares in a large range of heights in the solar atmosphere have been carried out. The physical state of the photosphere before solar flares and at their initial stage has been determined on the basis of the observations. We have observed and studied some variations of chromospheric thermodynamic parameters at the initial stage of a flare and a two-ribbon flare. Nonhomogeneous semiempirical models of the flare chromosphere and surge have been built for the moments of the flare observations. Our calculations in the framework of two-component chromospheric models point to a possible existence of some details with deep heating chromospheric layers. Some twist motions were observed in the active region photosphere and chromosphere. The temporal changes of the horizontal velocities in the kernel sites and their surroundings were of a wave character and were nearly synchronous throughout the whole height of the photosphere. A detailed analysis of the motion of matter initially in the low-temperature atmospheric layers and in the flare regions on the Sun is an important factor for understanding the processes of propagation of turbulence from the region of the primary energy release as a result of magnetic reunions in flares of various types. The study of the field of velocity of the flare area by observations in a wide spectral range enables us to verify the validity of existing ideas about the mechanisms of the transfer of flare energy.

PACS number(s): 95.55.Ev, 96.60.Mz

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