The Effect of Heat Conduction on the Formation of Coronal Condensations in the Solar Atmosphere

In this work, the evolution of oscillation instability in large-scale magnetic fields in the upper layers of the Sun’s convective zone is studied. The nonlinear phase of the Parker instability evolution is studied in the thin magnetic tube approximation for slow oscillation modes up to the saturation stage. The dynamics of magnetic structures emerging from the convective zone to the solar atmosphere was calculated taking into account the heating of the magnetic tube gas due to the effect of heat conduction along magnetic field lines. Two phases of the formation of solar prominences (coronal condensations) under conditions of the anomalously heated solar atmosphere are distinguished: the explosive phase of the magnetic field emission into the solar chromosphere with hypersonic velocities (about 300 km/s) and the phase of deceleration of emerging magnetic fields in the Sun’s corona. The stability of coronal condensations is preliminarily analyzed depending on their horizontal size in the solar atmosphere. The physical processes leading to the implementation of coronal transients (coronal mass ejections) in the solar atmosphere after the explosive phase of the magnetic field emission to the chromosphere are revealed.