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Information × Registration Number 0222U000052, 0120U100278 , R & D reports Title Possible mechanism of glow of solar flares: observation and numerical simulation popup.stage_title Head Kostik Roman I., Доктор фізико-математичних наук Registration Date 02-01-2022 Organization Main Astronomical Observatory of the National Academy of Sciences of Ukraine popup.description2 The object of research is the active regions on the solar surface (faculae). The purpose of the work is to justify the mechanism of glow of solar faculaes. The method of research is an analysis of simultaneous spectral, filter and spectropolarimetric observations of the active regions on the Sun surface obtained on a telescope VTT (Spain); mathematical modeling. Results and their novelty - as a result of processing and interpretation of observation data received by the project authors, a mechanism of glow of solar faculaes is substantiated. To the most significant results obtained during the implementation of the topic, you can include the following: 1. The magnetic field strength in the faculaes according to spectropolarimetric observations is determined. It is shown that the contrast (brightness) of the facula increases non-monotonously with an increase of the magnetic field strength B, and, starting from B = 140 mTl, it decreases. This is contrary to the currently accepted explanation of the increased brightness of facular regions as a result of the Wilson effect. This questioned the generally accepted to the present the mechanism of glow of solar faculaes - the so-called Wilson's effect as the only possible. 2. Contrast (brightness) of the faculae in the upper chromosphere depends heavily on the direction of distribution of sound waves in the atmosphere of the Sun. This result may indicate that in the active section of the solar surface of the sound wave can transfer energy from the photosphere to the chromosphere and, as a consequence, to change the contrast of the faculae. 3. Mathematical modeling within a three-dimensional magnetic-hydrodynamic model of the Sun atmosphere convincingly shows that the temperature in solar faculaes can really be higher than that of the surrounding atmosphere. In our opinion, this is a very important result, since they become more understandable changes in the solar constant during the 11-year cycle of activity by 0.1%. Product Description popup.authors Kostik Roman I. Osipov Sergiy M. Khomenko Olena V. Shukina Nataliya G. popup.nrat_date 2022-03-09 Close