Modeling of sunspot structures using simulations of axisymmetric MHD convection

We present our efforts on modeling solar pores and sunspots in 2D and 2.5D axisymmetric magneto-hydrodynamic (MHD) simulations of the upper layers of the Sun's convection zone. One goals of this work is to produce consistent, self-maintained, even if not fully realistic, models of concentrated, strong magnetic field in subsurface layers of the Sun. These models are important for understanding the mechanisms of magnetic field concentration in sunspots, and associated large-scale flow patterns. Also, these can be used as background models in acoustic wave propagation simulations for testing local helioseismology techniques and their performance and problems in magnetic regions. This study explores the parameters under which magnetic field can spontaneously concentrate, and the kind of flow patterns that form in these cases (for instance if there are inflows or outflow at the surface).