Some properties of convective motions in the upper solar atmosphere. II |
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Authors: | R I Kostyk |
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Institution: | 1.Main Astronomical Observatory,National Academy of Sciences of Ukraine,Kyiv,Ukraine |
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Abstract: | Using a three-dimensional hydrodynamical model of the solar atmosphere, we calculated profiles of the Fe I λ 639.361 nm and
Fe II λ 523.462 nm lines with consideration for deviations from the local thermodynamic equilibrium. We determined heights
for intensity contrast reversal and for velocity sign reversal of convective elements. Both of these parameters depend strongly
on the convective velocity and intensity measured in the continuum. The larger the parameters, the greater is the atmosphere
altitude where the reversal takes place. We compared all the calculated relations with the observations obtained at the German
Vacuum Tower Telescope in Izana (Tenerife, Spain). In our opinion, the 3D hydrodynamical model of the solar atmosphere satisfactorily
describes all the main features of observed convective velocities and intensities. |
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