What causes the 24-day period observed in solar flares?

Temmer, Manuela; Rybák, J.; Veronig, Astrid; Hanslmeier, A.

doi:10.1051/0004-6361:20041833

Cited by 3 publications

(2 citation statements)

References 23 publications

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“…Knaack et al (2005) provide evidence for a multitude of quasi-periodic oscillations of the photospheric magnetic field in this temporal range, suggesting that the 1.3 year period could be related to large-scale magnetic surges appearing in the 30-55 latitude belts during the maxima of the solar cycles 21-23. suggest that both 1.3 year and 155 days could be harmonics of the 11year cycle, without excluding a link with the solar dynamo via changes in the solar rotation. Analyzing solar flare data Temmer et al (2005) proposes that the appearance of active periods around 155 days might result from the superposition of predominant periods of 24 and 28 days, related with the solar rotation period.…”

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155-day Periodicity in solar cycles 3 and 4

et al. 2010

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The near 155 days solar periodicity, so called Rieger periodicity, was first detected in solar flares data and later confirmed with other important solar indices. Unfortunately, a comprehensive analysis on the occurrence of this periodicity during previous centuries can be further complicated due to the poor quality of the sunspot number time-series. We try to detect the Rieger periodicity during the solar cycles 3 and 4 using information on aurorae observed at mid and low latitudes. We use two recently discovered aurora datasets, observed in the last quarter of the 18th century from UK and Spain. Besides simple histograms of time between consecutive events we analyse monthly series of number of aurorae observed using different spectral analysis (MTM and Wavelets). The histograms show the probable presence of Rieger periodicity during cycles 3 and 4. However different spectral analysis applied has only confirmed undoubtedly this hypothesis for solar cycle 3. PACS: 96.50.Wx, 92.60.hw

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155-day Periodicity in solar cycles 3 and 4

et al. 2010

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“…To further investigate the solar North-South asymmetry, many solar activity indices have been thoroughly examined (Waldmeier 1971;Roy 1977;Swinson et al 1986;Yi 1992;Carbonell et al 1993;Oliver & Ballester 1994;Meunier et al 1997;Temmer et al 2002Temmer et al , 2006Hathaway et al 2003;Gigolashvili et al 2005;Zaatri et al 2006;Zolotova & Ponyavin 2006Donner & Thiel 2007;Chang 2008Chang , 2009Javaraiah 2008;Li 2010;Li et al 2010). Since it was established, the North-South asymmetry is also considered as one of the most interesting fea-326 Chang Figure 1.…”

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Latitudinal Distribution of Sunspots and Duration of Solar Cycles

Chang¹

2015

Journal of The Korean Astronomical Society

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Abstract:We study an association between the duration of solar activity and characteristics of the latitude distribution of sunspots by means of center-of-latitude (COL) of sunspots observed during the period from 1878 to 2008 spanning solar cycles 12 to 23. We first calculate COL by taking the areaweighted mean latitude of sunspots for each calendar month to determine the latitudinal distribution of COL of sunspots appearing in the long and short cycles separately. The data set for the long solar cycles consists of the solar cycles 12, 13, 14, 20, and 23. The short solar cycles include the solar cycles 15, 16, 17, 18, 19, 21, and 22. We then fit a double Gaussian function to compare properties of the latitudinal distribution resulting from the two data sets. Our main findings are as follows: (1) The main component of the double Gaussian function does not show any significant change in the central position and in the full-width-at-half-maximum (FWHM), except in the amplitude. They are all centered at ∼ 11• with FWHM of ∼ 5• . (2) The secondary component of the double Gaussian function at higher latitudes seems to differ in that even though their width remains fixed at ∼ 4• , their central position peaks at ∼ 22.1• for the short cycles and at ∼ 20.7• for the long cycles with quite small errors. (3) No significant correlation could be established between the duration of an individual cycle and the parameters of the double Gaussian. Finally, we conclude by briefly discussing the implications of these findings on the issue of the cycle 4 concerning a lost cycle.

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The Periodicity of High-Latitude Solar Activity

et al. 2006

Sol Phys

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The periodicity of high-latitude solar activity has been studied with the use of the Carte Synoptique solar filaments archive. The Morlet wavelet is utilized to analyze the periodicity of the number of solar filaments at latitudes over 50 • during Carrington solar rotations 876 -1823. For solar filaments at latitudes over 50 • , the most eminent periods are about 10.23 and 10.90 years, which correspond to the Schwabe period of high-latitude solar activity, and the these periods make-up a highly significant proportion of the time span considered. The periods of 1.3 and 1.7 years and the quasi-biennial 2 -3-year oscillation often mentioned in the literature are not found to be a feature of every solar cycle but seem to appear only from time to time.

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What causes the 24-day period observed in solar flares?

Cited by 3 publications

References 23 publications

155-day Periodicity in solar cycles 3 and 4

155-day Periodicity in solar cycles 3 and 4

Latitudinal Distribution of Sunspots and Duration of Solar Cycles

The Periodicity of High-Latitude Solar Activity

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