Diverging and Converging Flows around Sunspot Structures in Rotating and Non-Rotating Axisymmetric MHD Simulations

Details Diverging and Converging Flows around Sunspot Structures in Rotating and Non-Rotating Axisymmetric MHD Simulations Diverging and Converging Flows around Sunspot Structures in Rotating and Non-Rotating Axisymmetric MHD Simulations

2010-06-21

arxiv.org/abs/1006.4156v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

4 pages, 4 figures

Scientific paper

We present results on modeling solar pores and sunspots using 2D axisymmetric magneto-hydrodynamic (MHD) simulations. These models are helpful for understanding the mechanisms of magnetic field concentration in sunspots, and the large-scale flow patterns associated with them. The simulations provide consistent, self-maintained, although not fully realistic, models of concentrated magnetic field near the solar surface. In this paper, we explore under which conditions the associated flows are converging or diverging near the surface. We find that in most cases in which a stable, pore-like concentration of magnetic field forms, a configuration with converging over diverging flow is established.

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