Features of Convection in the Atmospheric Layers of the Solar Facula

Resumo

According to the data of complex 2D observations on the VTT telescope of the solar facula, a 3D model of the solar atmosphere in the facular region was obtained by solving the inverse radiative transfer problem in the Ba II 4554 A line. The magnetic field was estimated using the Stokes V profiles of the Fe I 15648 A line. The influence of magnetic field on photospheric convection was investigated: spatial variations in temperature and velocities at different heights were considered. It is shown that the mutual transformation of the mechanical and thermal energy of the solar plasma into magnetic energy occurs in the layers of the middle photosphere. The integral effect of a small-scale magnetic dynamo leads to lowering the temperature and slowing down the motion of the predominant downward flows in the layers of the middle photosphere in the facular regions with a strong field (greater than 1 kG), while there is an increase in temperature and acceleration of the motion of the predominant upward flows in the layers of the middle photosphere in the facular regions with a weak field (less than 1 kG). It is shown that the magnetic field of the facula stabilizes photospheric convection, and the small-scale magnetic dynamo causes a double temperature inversion in the photospheric layers of the facula.