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The influence of magnetic field on the propagation of 5-min oscillations in the solar atmosphere: the phase shifts. Russian. 2014 ;30(1):61-69.
. What mechanisms allow the 5-minute oscillations in the active regions of the solar surface to penetrate from the photosphere into the chromosphere?. Russian. 2015 ;31(4):45-53.
. Properties of convective motions in the upper solar atmosphere. I. Russian. 2010 ;26(5):26-40.
. Some properties of convective motions in the upper solar atmosphere. II. Russian. 2011 ;27(4):24-34.
. The effect of magnetic field on fine structure of convective motions in the solar atmosphere. Russian. 2012 ;28(4):3-14.
. Multicomponent simulation of emission of low-metallicity H II regions. Ukrainian. 2014 ;30(2):26-47.
. Modelling of H II region emission with bubble-like structure inside. Ukrainian. 2013 ;29(6):3-19.
. Modelling of H II region radiation surrounding the starburst knot taking into account the structures evolution formed by superwind. Ukrainian. 2017 ;33(2):3-23.
. Determination of secular polar motion from astronomical observations. The priority of O. Ya. Orlov. 2016 ;32(2):74-80.
. Fourier-components phase accumulation in the observation of an object through a turbulent atmosphere. I. Russian. 2011 ;27(6):52-63.
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