Changes in the solar summary magnetic flux with time, latitude and height

  • O.A. Andreeva Crimean Astrophysical Observatory
  • G.V. Rudenko Институт солнечно-земной физики СО РАН (ИСЗФ), а/я 291, Иркутск, Россия, 664033
  • N.N. Stepanian Crimean Astrophysical Observatory
  • V.G. Fainshtein Институт солнечно-земной физики СО РАН (ИСЗФ), а/я 291, Иркутск, Россия, 664033


The solar summary magnetic flux of each rotation was analyzed in 10-degree latitude zones. The summary flux is the sum of absolute values of the magnetic fluxes of “+” and “–” polarity in the longitudinal intervals 0–360° at heights from the photosphere to the source’s surface. Synoptic maps of the magnetic field of the Sun for 3 solar cycles (1975–2010 years) at five heights in the solar atmosphere served as basic data for the study. The latitudinal and height distribution of the summary magnetic flux and velocity of its variation over time were studied. Velocities of changes in the summary flux were measured as difference of a summary flux in the current rotation minus a flux in the previous rotation. The difference of fluxes refers to the previous rotation.

Periodic oscillations are visible in velocity of changes in the summary fluxes for the epoch of maximum activity during cycles 21, 22 and 23 per latitudinal zones –15° to + 15°, with the following characteristics:

 – Velocity oscillations during the period are symmetrically about zero.

– The amplitude of oscillation is about 0.5 of the average summary flux at heights H0 – H9.

– The average autocorrelation coefficient is 0.43 ± 0.05.

– The average period is 8.4 ± 1.6 Carrington rotations or 7.6 ± 1.4 months


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How to Cite
Andreeva O., Rudenko G., Stepanian N., Fainshtein V., 2016. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 112, no. 1, pp. 18-27. Available at: (Accessed: 1December2020)
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