Abstract
By combining quiet-region Fe XII coronal images from SOHO/EIT with magnetograms from NSO/Kitt Peak and from SOHO/MDI, we show that the population of network coronal bright points and the magnetic flux content of the network are both markedly greater under the bright half of the large-scale quiet corona than under the dim half. These results (1) support the view that the heating of the entire corona in quiet regions and coronal holes is driven by fine-scale magnetic activity (microflares, explosive events, spicules) seated low in the magnetic network, and (2) suggest that this large-scale modulation of the magnetic flux and coronal heating is a signature of giant convection cells.
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References
Beck, J. G., Duvall, T. L., Jr., and Scherrer, P. H.: 1998, Nature, 394, 653.
Falconer, D. A., Moore, R. L., Porter, J. G., and Hathaway D. H.: 1998, Ap.J., 501, 386.
Falconer, D. A., Moore, R. L., Porter, J. G., and Hathaway D.H.: 1999, in preparation for submission to Ap.J.
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Falconer, D.A., Moore, R.L., Porter, J.G. et al. Large-scale Coronal Heating, Clustering of Coronal Bright Points, and Concentration of Magnetic Flux. Space Science Reviews 87, 181–184 (1999). https://doi.org/10.1023/A:1005175812837
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DOI: https://doi.org/10.1023/A:1005175812837