3D MHD Simulations of Spontaneous Flow Ejections by Turbulent Convection into the Chromosphere

Dynamical interaction of the highly turbulent subsurface and the low atmosphere layers is a source of many observed phenomena on various scales in the solar chromosphere. We investigate the energetic and dynamical links between the turbulent convection and the chromosphere by using 3D radiative MHD simulations. Our simulations of quiet-Sun regions reveal ubiquitous formation of small-scale vortex tubes which can drive flow ejections into the chromosphere. The vortex tubes are formed through two basic mechanisms: convective instability inside the granules and the Kelvin-Helmholtz instability in the intergranular lanes. During their formation the vortex tubes become mostly vertical and usually can be detected in the intergranular lanes. Dispute their small scale the vortex tubes represent highly dynamical structures, which can capture surrounding magnetic field and easily penetrate into the atmosphere layers, producing quasi-periodic flow ejections, shocks and Alfven waves, and contribute to the chromosphere heating.