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

Rieger, E.; Share, G. H.; Forrest, D. J.; Kanbach, G.; Reppin, C.; Chupp, E. L.

doi:10.1038/312623a0

Cited by 407 publications

(312 citation statements)

References 2 publications

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“…We presented evidence above for r-mode oscillations [33] in the Homestake and GALLEX-GNO data that appear to be the origin of the well-known Rieger oscillation [31] and of similar "Rieger-type" oscillations [32] that have been discovered in recent years. We have therefore examined the possibility that peaks A and B may be related to such oscillations interpreted as r modes.…”

Section: Explanation For the Peak Frequenciesmentioning

confidence: 97%

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Evidence for solar neutrino flux variability and its implications

Caldwell

Sturrock

2005

Astroparticle Physics

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Although KamLAND apparently rules out Resonant-Spin-Flavor-Precession (RSFP) as an explanation of the solar neutrino deficit, the solar neutrino fluxes in the Cl and Ga experiments appear to vary with solar rotation. Added to this evidence, summarized here, a power spectrum analysis of the Super-Kamiokande data reveals significant variation in the flux matching a dominant rotation rate observed in the solar magnetic field in the same time period. Three frequency peaks, all related to this rotation rate, can be explained quantitatively. A Super-Kamiokande paper reported no time variation of the flux, but showed the same peaks, there interpreted as statistically insignificant, due to an inappropriate analysis. This modulation is small (7%) in the Super-Kamiokande energy region (and below the sensitivity of the Super-Kamiokande analysis) and is consistent with RSFP as a subdominant neutrino process in the convection zone. The data display effects that correspond to solar-cycle changes in the magnetic field, typical of the convection zone. This subdominant process requires new physics: a large neutrino transition magnetic moment and a light sterile neutrino, since an effect of this amplitude occurring in the convection zone cannot be achieved with the three known neutrinos. It does, however, resolve current problems in providing fits to all experimental estimates of the mean neutrino flux, and is compatible with the extensive evidence for solar neutrino flux variability.

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Section: Explanation For the Peak Frequenciesmentioning

confidence: 97%

“…with frequencies of about 2.4, 4.7, and 7.1 y −1 [31]. These periodicities may be attributed to r-mode oscillations [33] with spherical harmonic indices ℓ = 3, m = 1,2,3, giving frequencies ν = 2mν R /ℓ(ℓ + 1), where ν R is the sidereal rotation rate [ν(sid) = ν(syn) + 1].…”

Section: Review Of Past Evidencementioning

confidence: 99%

Evidence for solar neutrino flux variability and its implications

Caldwell

Sturrock

2005

Astroparticle Physics

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“…A 154-day periodicity was first reported in gamma-ray flares detected on the Solar Maximum Mission [Rieger et at., 1984]. Subsequently, this periodicity has been reported in other flare data sets (see Bai and $turrock, [1993] and references therein) and also for active region parameters [Lean and Brueckner, 1989] including sunspot areas [Lean, 1990].…”

Section: Introductionmentioning

confidence: 99%

Interplanetary magnetic field periodicity of ∼153 days

Cane

Richardson

Rosenvinge

1998

Geophysical Research Letters

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“…In our Homestake article [1], we drew attention to the Rieger oscillation [40] (with a period of about 154 days) and related oscillations, which we here refer to as "Rieger-type" oscillations (for instance, oscillations with 72 day period and 51 day period) [41 -45]. The nature of these oscillations is still a matter of debate [45].…”

Section: Appendix B Indication Of Modulation At R-mode Frequenciesmentioning

confidence: 99%

Comparative analysis of GALLEX and GNO solar neutrino data

Sturrock

Caldwell

Scargle

2006

Astroparticle Physics

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Since the GALLEX and GNO datasets were derived from closely related experiments, there is a natural tendency to merge them. This is perhaps appropriate for any analysis based on the hypothesis that the solar neutrino flux is constant, but it is not necessarily appropriate for an analysis that allows for possible variability, since the GALLEX and GNO experiments belong to different solar cycles. Moreover, we find significant differences between the GALLEX and GNO datasets. It appears, from inspection of the time series and histograms, that GNO measurements are compatible with the assumption that the solar neutrino flux is constant, but GALLEX measurements are not. Furthermore, power-spectrum analysis yields evidence of rotational modulation in GALLEX data but not in GNO data. We compare our results with those of Pandola, who claims that GALLEX-GNO data show no evidence for variability.

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

Cited by 407 publications

References 2 publications

Evidence for solar neutrino flux variability and its implications

Evidence for solar neutrino flux variability and its implications

Interplanetary magnetic field periodicity of ∼153 days

Comparative analysis of GALLEX and GNO solar neutrino data

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