Abstract
A cross-correlation analysis of coronal green line intensity (5303 Å) and interplanetary magnetic field polarity for the period 1947–1970 shows that the coronal features are organized in a constant pattern with respect to the 4-sector structure through the solar cycle. A sudden inversion of the coronal pattern with respect to the sector structure takes place at the solar minima. The high emission regions of the green corona are located near the solar magnetic sector boundaries having polarities (−, +), (+, −), (−, +) during cycles 18, 19, 20 respectively in the northern hemisphere, and (+, −), (−, +), (+, −) in the southern hemisphere.
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References
Antonucci, E. and Svalgaard, L.: 1974, Solar Phys., 34, 3.
Rosenberg, R. L. and Coleman, P. J., Jr.: 1969, J. Geophys. Res. 74, 5611.
Svalgaard, L.: 1972, Dan. Meteorol. Inst., Geophys. Pap. 29.
Wilcox, J. M.: 1968, Space Sci. Rev. 8, 258.
Wilcox, J. M., Severny, A., and Colburn, D. S.: 1969, Nature 224, 353.
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ESRO/NASA Fellow, on leave from Torino University, Italy.
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Antonucci, E. Eleven-years inversion of the green corona emission. Sol Phys 34, 471–476 (1974). https://doi.org/10.1007/BF00153683
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DOI: https://doi.org/10.1007/BF00153683