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- Title
Height stratification and polar reversal of the Sun’s magnetic fields in cycles 21–23.
- Authors
Stepanyan, N. N.; Akhtemov, Z. S.; Fainshtein, V. G.; Rudenko, G. V.
- Abstract
Using calculations of the magnetic field in the solar atmosphere in the potential approximation, it is shown that, (1) as distance R from the Sun’s center grows, the area of the positive magnetic field ( S+field) in 10-deg latitude zones tends to 100% (0%) in the neighborhood of the solar minimum. At the distance R = 2.5 R⊙( R⊙ is the solar radius), these values of the positive field are observed during ≈(12–55) Carrington rotations (CRs) for solar minima between neighboring cycles; (2) polar magnetic field reversals can occur repeatedly. Note that a polar reversal at large heights ends by 6–16 Carrington rotations earlier than on the Sun’s surface. On the Sun’s surface, a field polar reversal begins earlier at lower latitudes than at high ones; (3) for each longitude at different Rs and separately for each solar hemisphere the radial component of the field was averaged on synoptic maps in the 0°–40° latitude range. It is established that the TR rotation periods of the boundaries between the sectors (areas of longitudes with the same sign of the averaged field) can be shorter than, longer than, and equal to Carrington solar rotation period TCR. It turned out that boundaries with TR < TCR are observed at all heights, while boundaries with TR > TCR are observed at relatively small heights.
- Subjects
GEOMAGNETIC reversals; SOLAR magnetic fields; MAGNETIC fields in the solar corona; MATHEMATICAL models; MAGNETIC fields; SOLAR atmosphere
- Publication
Geomagnetism & Aeronomy, 2013, Vol 53, Issue 7, p957
- ISSN
0016-7932
- Publication type
Article
- DOI
10.1134/S0016793213080252