Photospheric Magnetic Field of the Sun: Two Patterns of the Longitudinal Distribution

Vernova, E. S.; Tyasto, M. I.; Baranov, D. G.

doi:10.1007/s11207-007-9018-2

Cited by 10 publications

(10 citation statements)

References 29 publications

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“…An analogous pattern of the active longitudes was discovered for coronal mass ejections by Skirgiello (2005). In a manner similar to the results of Vernova et al (2004) and Vernova, Tyasto, and Baranov (2007), two nearly antipodal longitudes dominated alternately: the domination of the longitude 180 • coincided with the ascending phase and the maximum, while the domination of the longitude 30 • coincided with the descending phase and the minimum of the solar cycle.…”

Section: Introductionsupporting

confidence: 78%

“…We found it to be essential to divide a 22-year magnetic cycle into four intervals where the polarities of the local and global magnetic fields are constant when we considered the longitudinal distribution of sunspots (Vernova et al, 2004) and of photospheric magnetic fields (Vernova, Tyasto, and Baranov, 2007). The longitudinal distribution for the ascending phase and the maximum sharply differ from the longitudinal distribution for the descending phase and the minimum of the solar cycle.…”

Section: Introductionmentioning

confidence: 99%

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Photospheric Magnetic Field: Relationship Between North–South Asymmetry and Flux Imbalance

Vernova¹,

Tyasto²,

Baranov³

2014

Coronal Magnetometry

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Photospheric magnetic fields were studied using the Kitt Peak synoptic maps for 1976 − 2003. Only strong magnetic fields (B > 100 G) of the equatorial region were taken into account. The north-south asymmetry of the magnetic fluxes was considered as well as the imbalance between positive and negative fluxes. The north-south asymmetry displays a regular alternation of the dominant hemisphere during the solar cycle: the northern hemisphere dominated in the ascending phase, the southern one in the descending phase during Solar Cycles 21 − 23. The sign of the imbalance did not change during the 11 years from one polar-field reversal to the next and always coincided with the sign of the Sun's polar magnetic field in the northern hemisphere. The dominant sign of leading sunspots in one of the hemispheres determines the sign of the magneticflux imbalance. The sign of the north-south asymmetry of the magnetic fluxes and the sign of the imbalance of the positive and the negative fluxes are related to the quarter of the 22-year magnetic cycle where the magnetic configuration of the Sun remains constant (from the minimum where the sunspot sign changes according to Hale's law to the magnetic-field reversal and from the reversal to the minimum). The sign of the north-south asymmetry for the time interval considered was determined by the phase of the 11-year cycle (before or after the reversal); the sign of the imbalance of the positive and the negative fluxes depends on both the phase of the 11-year cycle and on the parity of the solar cycle. The results obtained demonstrate the connection of the magnetic fields in active regions with the Sun's polar magnetic field in the northern hemisphere.

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Section: Introductionsupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Photospheric Magnetic Field: Relationship Between North–South Asymmetry and Flux Imbalance

Vernova¹,

Tyasto²,

Baranov³

2014

Coronal Magnetometry

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“…It was earlier shown for three solar cycles that the localization of active longitudes of magnetic fields depends on a phase of solar cycle (Vernova, Tyasto, and Baranov, 2007). In longitudinal distribution of the photospheric magnetic fields two specific periods appear: (a) the phase of ascent-maximum (AM) and The time moments dividing the two specific intervals (ascent-maximum and descent-minimum) are the important critical points of the magnetic solar cycle.They coincide with the change of the polar field sign near the maximum of solar cycle and with the change of signs of the leading sunspots at the minimum of solar cycle (according to the Hale law).…”

Section: Resultsmentioning

confidence: 99%

Nonaxisymmetric Component of the Solar Photospheric Magnetic Field

et al. 2019

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The longitudinal asymmetry of the photospheric magnetic field distribution is studied on the basis of the data of the Kitt Peak National Solar Observatory (synoptic maps for the period 1976-2016). The method of vector summing of magnetic fields is used, which allows to decrease the influence of the stochastic components uniformly distributed over the whole longitude interval, and to stress a steady non-axisymmetric component of the field. The distributions of magnetic fields of different intensity are considered separately for the strong (B > 50 G), weak (B < 5 G) and medium (50 > B > 5 G) fields. It is shown that the longitudinal asymmetry for all groups of fields changes in phase with the 11-year cycle of solar activity. The asymmetry of strong and medium fields changes in phase with magnetic fluxes of these fields, while the asymmetry of weak fields is in antiphase with the flux of weak fields. The distributions of strong and medium magnetic fields over the longitude are similar in the shape: The maximum of distribution is located at the longitude ∼ 180 • during the period of ascent-maximum of solar cycle and at the longitude ∼ 0 • /360 • during the period of descent-minimum. The weak fields exhibit the opposite picture: the maximum of their distribution is always observed at the longitude, where the strong and medium fields show minimum.

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“…Для этого используются синоптические карты фотосферного магнитного поля обсерватории Китт Пик. Ранее [2] мы рассматривали долготную асимметрию магнитных полей по данным прибора KPVT (19762003 гг.). В настоящей работе использованы также данные прибора SOLIS/VSM, что позволило распространить исследование вплоть до 2017 г., т.е.…”

Section: Doi: 1031725/0552-5829-2018-95-98unclassified

“…Ранее было показано для трех солнечных циклов, что локализация активной долготы зависит от фазы солнечного цикла [2]. В долготном распределении сильных фотосферных магнитных полей проявляются два характерных периода: (a) фазы подъем-максимум (AM) и (b) фазы спад- минимум (DM).…”

Section: Doi: 1031725/0552-5829-2018-95-98unclassified