Time-Latitudinal Dynamics of Magnetic Fields and the Green Corona Over Three Solar Cycles

Minarovjech, M.; Rusin, V.; Санига, Метод

doi:10.1007/s11207-007-0239-1

Cited by 6 publications

(15 citation statements)

References 17 publications

(1 reference statement)

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“…They prepare a new synoptic chart (the processed longitudinally averaged magnetic flux) as shown in the lower part of their Figure 1, and it is shown here again as Figure 7. It can be easily seen from Figure 7 that the boundaries (branches) between the opposite polarities of the magnetic field split off the “longitudinally averaged magnetic field” butterfly pattern at midlatitudes and migrate from there toward the poles [ Minarovjech et al , 2007]. Comparison between the absolute values of magnetic field intensities and the green corona local maxima is shown in their Figure 3 and here again in Figure 8, and the time‐varying component of the green corona and its meriodional migration correlate well with the magnetic‐field distribution and their flows, as indicated in Figure 8.…”

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

“…Comparison between the absolute values of magnetic field intensities and the green corona local maxima is shown in their Figure 3 and here again in Figure 8, and the time‐varying component of the green corona and its meriodional migration correlate well with the magnetic‐field distribution and their flows, as indicated in Figure 8. The green corona intensities are very intimately connected with the distribution of solar local magnetic flux and mimic its development over a solar cycle, and further, a direct physical coupling the photospheric magnetic fields and the green corona, discovered in the middle and low heliographic latitudes, applies well also to polar regions [ Minarovjech et al , 2007]. Thus, a full‐disk activity cycle for the solar surface magnetic fields is proposed to consist of two successive normal cycles as well: a high‐latitude activity cycle following a low‐latitude activity cycle.…”

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

“…The dashed lines correspond to 75°, above which the values of the magnetic field may be unreliable, because they are radial values inferred from a longitudinal magnetograph. Figure 7 is originally from Minarovjech et al [2007] (with kind permission of Springer Science and Business Media).…”

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

“…Meridional migrations for the magnetic fields from the bottom of Figure 7 (gray color scale) and the green corona (green color). Figure 8 is originally from Minarovjech et al [2007] (with kind permission of Springer Science and Business Media).…”

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

“…The velocity of the poleward migration of solar activity is in range of several to tens meters per second. It is 10 to 25 m s −1 for filament activity [ Minarovjech et al , 1998b] or 4 to 29 m s −1 [ Makarov and Sivaraman , 1989], several meters per second for the green‐corona intensities [ Minarovjech et al , 2007], 7 to 20 m s −1 for the surface magnetic fields.…”

Section: Fine‐scale Characteristics Of Full‐disk Activity Cyclesmentioning

confidence: 99%

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Cyclic behavior of solar full‐disk activity

Gao

et al. 2008

J. Geophys. Res.

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In order to describe the cyclic behavior of solar full‐disk activity (the surface magnetic fields, filaments, the green Fe XIV, 5303Å corona local maxima intensities, and torsional oscillations), we propose a new concept, a “full‐disk activity cycle,” which consists of two successive normal cycles: a high‐latitude activity cycle following a low‐latitude activity cycle. When solar activity begins to progress into a full‐disk activity cycle, it latitudinally rushes to the poles, starting from middle latitudes (about 40°) at about a normal cycle minimum. At the solar poles, magnetic polarity reversal takes place on both the solar hemispheres, and opposite reversals occur on the opposite hemispheres; resultingly, the new appearing magnetic polarity at high latitudes on a hemisphere will become the leading magnetic polarity of regions at low latitudes on the same hemisphere in the following normal cycle. After the latitudinal drift of solar activity reaches the solar poles at about the maximum time of the normal cycle, solar activity begins to latitudinally migrate in a reverse direction; it moves toward the equator continually till almost arriving at the solar equator and lasting for about 1.5 normal cycles. When a full‐disk activity cycle progresses from a high‐latitude activity cycle into a low‐latitude activity cycle, the next full‐disk activity cycle begins. Two successive full‐disk activity cycles have a normal cycle overlapped in time but are spatially separated. The characteristics of full‐disk activity cycles are summarized as well. At present we do not know why a full‐disk activity cycle begins at midlatitudes; it is perhaps related with solar differential rotation. Further work is required to uncover the physical mechanisms behind the concept.

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Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

Section: Solar Full‐disk Activity Cyclementioning

confidence: 99%

Section: Fine‐scale Characteristics Of Full‐disk Activity Cyclesmentioning

confidence: 99%

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Cyclic behavior of solar full‐disk activity

Gao

et al. 2008

J. Geophys. Res.

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Coronal Mass Ejections, Magnetic Fields, and the Green Corona in Cycle 23

2008

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We study a time -latitudinal distribution of CMEs observed by the SOHO spacecraft, their projected speeds and associated magnetic fields, as well as the north -south (N -S) asymmetry of solar surface magnetic fields, and the coronal green line intensities. We have found that (a) there exists an intricate relation between the average projected velocity of CMEs and the mean value of large-scale magnetic fields; (b) there exists a pronounced N -S asymmetry in both the distribution and the number of CMEs; (c) this asymmetry is in favor of the northern hemisphere at the beginning of the cycle, and of the southern hemisphere from 2001 onward, being, in fact, (d) closely related with the N -S asymmetry in the distribution of large-scale magnetic fields and the coronal green line intensities.

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Time‐Latitude Distribution of Prominences for 10 Solar Cycles: A Study Using Kodaikanal, Meudon, and Kanzelhohe Data

Chatterjee

Hegde

Banerjee

et al. 2020

Earth and Space Science

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Solar prominences are structures of importance because of their role in polar field reversal. We study the long‐term variation of the time latitude distribution of solar prominences in this article. To accomplish this, we primarily used the digitized disc‐blocked Ca II K spectroheliograms as recorded from Kodaikanal Solar Observatory for the period of 1906–2002. For improving the data statistics we included full disc H α images from Meudon and Kanzelhohe Observatory, which are available after 1980. We developed an automated technique to identify the latitudinal locations of prominences in daily images from all three data sets. Derived time‐latitude distribution clearly depicted poleward migration of prominence structures for 10 cycles (15–24). Unlike previous studies, we separated the rate of poleward migration during onset and near pole, using piece‐wise linear fits. In most cases, we found acceleration in poleward migration with the change occurring near ±70° latitudes. The derived migration rates for such large number of solar cycles can provide important inputs toward understanding polar field buildup process.

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Time-Latitudinal Dynamics of Magnetic Fields and the Green Corona Over Three Solar Cycles

Cited by 6 publications

References 17 publications

Cyclic behavior of solar full‐disk activity

Cyclic behavior of solar full‐disk activity

Coronal Mass Ejections, Magnetic Fields, and the Green Corona in Cycle 23

Time‐Latitude Distribution of Prominences for 10 Solar Cycles: A Study Using Kodaikanal, Meudon, and Kanzelhohe Data

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