A 154-day periodicity in the occurrence of hard solar flares?

@article{Rieger1984A1P,
  title={A 154-day periodicity in the occurrence of hard solar flares?},
  author={Erich Rieger and Gerald Harvey Share and David J. Forrest and Gottfried Kanbach and Claus Reppin and Edward L. Chupp},
  journal={Nature},
  year={1984},
  volume={312},
  pages={623-625}
}
Since the launch of the Solar Maximum Mission (SMM) satellite on 1980 February 14, the Gamma-Ray Spectrometer (GRS)1 has been monitoring the Sun in the energy range 0.3–100 MeV. Because of its large geometric area and good spectral resolution, the GRS has provided unprecedented spectral and temporal information about solar flares, of which 139 have been monitored. We report here on an analysis of the temporal distribution of these high-energy events to provide information on solar activity and… 
Study of periodicities of solar nuclear gamma ray flares and sunspots
Here we have carried out a power-spectrum analysis of solar nuclear gamma-ray (NGR) flares observed by SMM and HINOTORI satellites. The solar NGR flares show a periodicity of 152 days, confirming the
The 154-day and related periodicities of solar activity as subharmonics of a fundamental period
IN 1984 a periodicity of 154 days was found in the record of solar flare activity1 from 1980 to 1983. Since then, the same periodicity has been found in many different measures of solar flare
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A periodicity near 154 days was discovered in the number of high-energy solar flares detected by Solar Maximum Mission (SMM) and Geosynchronous Operational Environmental Satellites (GOES) during the
Early stages of solar flares - Current status of our understanding and opportunities for future observations
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X-ray emission from the Sun fluctuates as a result of occasional flare events. We have calculated the power spectra of the solar soft X-ray variations using the photometric data of the GOES 6
Periodic behaviour of solar flare activity
The periodic nature of solar activity has been studied using parameters such as the sunspot Wolf numbers, calcium plage areas and flare indices. The magnitude of the solar activity based on these
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CORONAL holes are large-scale structures of lower density and temperature in the solar corona. They appear as large dark features in X-ray and radio images, and as bright areas in infrared He I
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