Abstract
Abstract—From 2D-spectral observation data of a quiet region of the solar disk center in the Fe I λ 557.609 nm line, 3D hydrodynamic models of photospheric jets are built by solving the inverse radiative transfer problem. The obtained models describe thermodynamic parameters and the complete velocity field (vertical and horizontal). It is shown that the photospheric jets under consideration arise from the interaction of the surrounding environment with the field of the magnetic tube. The jets are located in a region of a unipolar magnetized downflow at the impact point of two horizontal flows, and they tend to occur at the edge of magnetic tubes. The observed gas velocities are subsonic in downflows of the jets. Energy release in the photospheric jets is predominantly localized in the middle photosphere layers, where the excess pressure is maximal. Compared with the surrounding media, mass density in the jets is significantly increased in the upper layers and slightly decreased in the lower layers of the photosphere.
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