Plasma flows in the quiet solar chromosphere-corona transition region

This article is devoted to solving the problem of the plasma temperature distribution along a magnetic tube, one end of which is in the chromosphere, while the other is in the corona. The plasma temperature dependences of the density, pressure, and velocity of plasma are determined for various velocities of the plasma flow, which are given at the lower boundary of the transition region. In the case where gravitation can be neglected, these dependences are derived in the analytical form. The existence of three velocity ranges is demonstrated, for which: (a) the excitation of shock waves in the transition region is possible, (b) the transition region can be considered in the classical collisional approximation, and (c) the plasma heating process is close to the $p = \text{const}$ mode and the calculated hard ultraviolet radiation coincides well with modern satellite observations. Based on the obtained results, we concluded that generally in the presence of plasma flows, the quiet transition region between the corona and the chromosphere should be considered in the classical approximation of Coulomb collisions.