Midterm periods of solar filaments

Zou, Peng; Li, Qixiu

doi:10.1002/2014ja020304

Cited by 11 publications

(5 citation statements)

References 78 publications

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“…A period of ∼1.2 years is found in our study which can be inferred to be the ∼1.3 years periodicity observed in geomagnetic activity (Mursula & Zieger 2000), oscillation in Solar wind (Richardson et al 1994), velocity of solar wind (Li et al 2017), solar filament (Zou & Li 2014) and rate of internal rotation near the base of the solar convection layer (Howe et al 2000). On other hand ∼1.76 years period is related to the ∼1.7 years periodicity observed in the intensity of cosmic ray (Kato et al 2003), velocity of solar wind (Li et al 2017) and solar filament (Zou & Li 2014). These periods are also considered for understanding the behavior of magnetic field emergence and magnet-ic cycle of the Sun (Valdés-Galicia et al 1996).…”

Section: Resultssupporting

confidence: 73%

“…Mei et al (2018) also found these periods in 10.7 cm solar radio flux as well as sunspot area data and suggested that the observed periods may be due to the flow of magnetic flux generated inside the Sun from the Sun's photosphere to corona. Zou & Li (2014) suggested that the ∼1.2 years period may be one of the sub-harmonics 1 8 × 11 = 1.3 of the dominant 11 years solar cycle. Li et al (2017) also pointed out that the lifetime of the equilateral dipole field of the Sun is very close to the period around ∼1.76 years.…”

Section: Resultsmentioning

confidence: 99%

“…This period was also found in other solar indices like hard X-ray peak rate (Bai & Sturrock 1987;Dennis 1985;Verma & Joshi 1987), Hα flare importance (Ichimoto et al 1985), 10.7-cm radio peak flux (Kile & Cliver 1991;Roy et al 2019) etc. ; (ii) 84 days period was observed in flare data during solar cycle 20 (Bai & Sturrock 1991); (iii) 323 days periodicity was found in sunspot number as well as area (Oliver et al 1992); (iv) 1.3 years periodicity was observed in geomagnetic activity (Mursula & Zieger 2000), solar wind oscillation (Richardson et al 1994), solar wind velocity (Li et al 2017), solar filament (Zou & Li 2014) and rate of internal rotation near base of the solar convection layer (Howe et al 2000); (v) 1.7 years periodicity was found in the intensity of cosmic ray (Kato et al 2003), velocity of solar wind (Li et al 2017) and solar filament (Zou & Li 2014). The Sun also exhibits short-term (below 27 days) periodicity which mainly deals with spatial organization compare to temporal organization of the solar activity.…”

Section: Introductionmentioning

confidence: 95%

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Chaos and Periodicities in Solar Flare Index from Kandilli Observatory during 1976–2014

Roy

Prasad

Ghosh

et al. 2020

Res. Astron. Astrophys.

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The Solar Flare Index is regarded as one of the most important solar indices in the field of solarterrestrial research. It has the maximum effect on Earth of all other solar activity indices and is being considered for describing the short-lived dynamo action inside the Sun. This paper attempts to study the short as well as long-term temporal fluctuations in the chromosphere region of the Sun using the Solar Flare Index. The daily Solar Flare Index for Northern, Southern Hemisphere and Total Disk are considered for a period from January 1976 to December 2014 (total 14 245 days) for chaotic as well as periodic analysis. The 0–1 test has been employed to investigate the chaotic behavior associated with the Solar Flare Index. This test revealed that the time series data is non-linear and multi-periodic in nature with deterministic chaotic features. For periodic analysis, the Raleigh Power Spectrum algorithm has been used for identifying the predominant periods within the data along with their confidence score. The well-known fundamental period of 27 days and 11 years along with their harmonics are well affirmed in our investigation with a period of 28 days and 10.77 years. The presence of 14 days and 7 days periods in this investigation states the short-lived action inside the Sun. Our investigation also demonstrates the presence of other mid-range periods including the famous Rieger type period which are very much confirming the results obtained by other authors using various solar activity indicators.

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Section: Resultssupporting

confidence: 73%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 95%

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Chaos and Periodicities in Solar Flare Index from Kandilli Observatory during 1976–2014

Roy

Prasad

Ghosh

et al. 2020

Res. Astron. Astrophys.

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“…Other periodicities, from several to hundreds of days-for example, 13.5, 120, and 276 days-as well as the annual period, have also been determined (Rybák & Dorotovič 2002;Bai 2003;Zou & Li 2014;Kolotkov et al 2015;Xiang & Kong 2015;Deng et al 2016;Chowdhury et al 2013).…”

Section: Introductionmentioning

confidence: 98%

“…A lot of studies have been reported that the 1.3 and 1.7 year periodicities indeed exist in the solar interior, the atmospheres of the Sun, and the interplanetary space (e.g., Howe et al 2000;Singh et al 2012;Zou & Li 2014;Kudela et al 2002;Chowdhury et al 2013). Furthermore, they are associated with the basic process of solar dynamos, and can be clearly observed in the Sun.…”

Section: Introductionmentioning

confidence: 99%

Midterm Periodicity Analysis of the Mount Wilson Magnetic Indices Using the Synchrosqueezing Transform

Feng

Liu

Wang

et al. 2017

ApJ

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A novel time-frequency technique, called the synchrosqueezing transform (SST), is used to investigate the midterm periodic variations of magnetic fields on the solar surface. The Magnetic Plage Strength Index (MPSI) and the Mount Wilson Sunspot Index (MWSI), measured daily by the Mount Wilson . The short-, mid, and longer-term periodicities are represented and decomposed by the SST with hardly any mode mixing. This demonstrates that the SST is a useful time-frequency analysis technique to characterize the periodic modes of helioseismic data. Apart from the fundamental modes of the annual periodicity, ∼27 day rotational cycle and ∼11 year solar cycle, the SST reveals several midterm periodicities in the two magnetic activity indices, specifically, ∼157 day (i.e., Rieger-type periodicity), and ∼1.3 and 1.7 years. The periodic modes, with 116.4 and 276.2 day periodicity in the MPSI, with 108.5 and 251.6 day periodicity in the MWSI, and the 157.7 day periodicity in the two indices, are in better accord with those significant periodicities derived from the Rossby waves theoretical model. This study suggests that the modes are caused by the Rossby waves. For the 1.30 and 1.71 year periodicity of the MPSI, and the 1.33 and 1.67 year periodicity of the MWSI, our analysis infers that they are related to those periodicity with the same timescale in the interior of the Sun and in the high atmospheric layers.

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Hydrogen Lyman-Alpha Periodicity Behaviour During Various Solar Cycles

Kotzé

2023

Astrophys Space Sci

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The temporal behaviour of various periodicities of hydrogen Lyman-alpha (Ly-$\alpha $ α ) between 1950 and 2020 have been analysed using Lomb-Scargle and Morlet wavelets spectral analysis techniques. Daily mean values of Ly-$\alpha $ α radiance (https://lasp.colorado.edu/lisird/data/composite_lyman_alpha/) for each individual year were used in this investigation to obtain the temporal behaviour of particularly the Rieger periodicity (150–180 days), the synodic solar rotation periodicity ($\approx27$ ≈ 27 days) as well as the elusive 13.5-day periodicity. Results obtained showed that the Rieger periodicity dominates at solar maximum during strong solar cycle conditions (Cycles 19, 21, 22, and 23), while the $\approx27$ ≈ 27 -day periodicity is in most cases dominant during solar minima. On the other hand, the 13.5-day periodicity only appears above the 95% statistical confidence level during solar maxima of Cycles 19, 21, 22 and 24. Contrary to all previous Cycles since 1950, the 13.5-day periodicity appears exceptionally strong and above the 95% confidence level during the downward and minimum phases of Cycles 23 (2006) and 24 (2016) when its power exceeds that of the 27-day periodicity. This peculiar behaviour of the 13.5-day periodicity in Ly-$\alpha $ α can probably be attributed to the anomalous asymmetrical structure of the solar magnetic field during Cycles 23 and 24.

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Midterm periods of solar filaments

Cited by 11 publications

References 78 publications

Chaos and Periodicities in Solar Flare Index from Kandilli Observatory during 1976–2014

Chaos and Periodicities in Solar Flare Index from Kandilli Observatory during 1976–2014

Midterm Periodicity Analysis of the Mount Wilson Magnetic Indices Using the Synchrosqueezing Transform

Hydrogen Lyman-Alpha Periodicity Behaviour During Various Solar Cycles

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