Abstract
We present results from numerical modeling of emerging flux regions on the solar surface. The modeling was carried out by means of three-dimensional (3D) radiative MHD simulations of the rise of buoyant magnetic flux tubes through the convection zone and into the photosphere. Due to the strong stratification of the convection zone, the rise results in a lateral expansion of the tube into a magnetic sheet, which acts as a reservoir for small-scale flux emergence events at the scale of granulation. The interaction of the convective downflows and the rising magnetic flux tube undulates it to form serpentine field lines that emerge into the photosphere. Observational characteristics, including the pattern of the emerging flux regions, the cancellation of surface flux and associated high-speed downflows, the convective collapse of photospheric flux tubes, the appearance of anomalous darkenings, the formation of bright points, and the possible existence of transient kilogauss horizontal fields are discussed in the context of new observations from the Hinode Solar Optical Telescope. Implications for the local helioseismology of emerging flux regions are also discussed.
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