Abstract
Autocorrelation and cross-correlation techniques have been applied to obtain quantitative information about the dynamics of magnetic flux on the solar surface. The speed of network magnetic elements and the diffusion coefficient associated with their random motion is derived. The speed is found to be about 0.1 km s−1, independent of activity level. However, the diffusion coefficient shows a strong activity dependence: it is about 370–500 km2 s−1in the quiet network and 135–210 km2 s−1in the enhanced network. It is found that the lifetime of the enhanced network relative to the quiet network is compatible with that suggested by a comparison of their respective diffusion coefficients. This supports the proposition that a diffusion-like dispersion of magnetic flux is the dominant factor in the large-scale, long-term evolution of the network.
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Srikanth, R., Singh, J. & Raju, K. The Chromospheric Network – (A) Network Evolution Viewed as a Diffusion Process. Solar Physics 187, 1–9 (1999). https://doi.org/10.1023/A:1005168001758
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DOI: https://doi.org/10.1023/A:1005168001758