Numerical Study of Morphology of Turbulent Convection

Tian Chunlin, chunlin.tian@helsinki.fi, Department of Physics, Univseristy of Helsinki, Finland
Petrovay Kristof, Department of Astronomy, ELTE

Abstract
Magnetized turbulent convection plays a very important role in determining the structure and thus the evolution of stars, especially the dynamical process of all kinds of activities. A full understanding of magnetoconvection is not only necessary for explaining the observed solar activities and predicting the upcoming solar events, but also very useful to interpret the near-future observation of faraway stars. The numerical study of turbulent magnetoconvection achieved so far can be grouped into two categories: expensive, fascinating realistic simulations and intuitive idealized models. There is big gap in parameter regime between these two kinds of study. We performed a serial of study to fill this gap. In this talk, we present some selected results of morphological properties of magnetized turbulent convection. They might be useful to understand the sub-structure of the observed Sunspots.