Abstract
It is shown that improved solar surface magnetogram resolution may make possible the study of the solar surface magnetic field spectrum's two-point correlation function two-dimensional Fourier transform. How the spectrum can be calculated from flux-tube models is explained, and the nature of information about the spatial and size distribution of the flux tubes that may be extracted from the observed spectrum is discussed in detail. It is demonstrated that specific spectrum predictions can be obtained from existing models on the basis of several plausible assumptions. It is noted that bipolar regions involving only small-scale tubes would have a different correlation function than larger-scale features, and that the solar cycle introduces anisotropies in the correlation function.
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