Abstract
A convective field of intensities and velocities between the levels of continuum origination and the temperature minimum is investigated based on spectral observations of iron lines performed near the center of the solar disc using the 70-cm German vacuum tower telescope (VTT) located at del Teide observatory of the Institute of Astrophysics on the Canaries (Tenerife island). Convective elements in the process of their upward and downward motion change with height not only the sign of the relative contrast but also the direction of motion. The height at which this reversal occurs strongly depends on the velocity and contrast of the convective elements which they had at the level of continuous spectrum formation. On average, the reversal of the velocity takes place at the height of 240 ± 130 km, and that of the contrast occur at the height of 200 ± 65 km.
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Original Russian Text © R.I. Kostyk, 2010, published in Kinematika i Fizika Nebesnykh Tel, 2010, Vol. 26, No. 5, pp. 26–40.
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Kostyk, R.I. Peculiarities of convective motions in the upper solar atmosphere. I. Kinemat. Phys. Celest. Bodies 26, 233–241 (2010). https://doi.org/10.3103/S0884591310050028
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DOI: https://doi.org/10.3103/S0884591310050028