Viewing the 'rush to the poles' through phase analysis
| Autor: | Nanbin Xiang, Defang Kong, Genmei Pan |
|---|---|
| Rok vydání: | 2014 |
| Předmět: |
Solar minimum
Physics Phase (waves) Astronomy and Astrophysics Solar maximum Atmospheric sciences Solar prominence Latitude Protein filament Space and Planetary Science Physics::Space Physics Astrophysics::Solar and Stellar Astrophysics Polar Astrophysics::Earth and Planetary Astrophysics Continuous wavelet transform |
| Zdroj: | Publications of the Astronomical Society of Japan. 66:28 |
| ISSN: | 2053-051X 0004-6264 |
| DOI: | 10.1093/pasj/pst029 |
| Popis: | At mid and low heliographic latitudes, filament activity shifts equatorward starting from the beginning of the solar cycle. At high latitudes, it migrates poleward. Solar filaments exhibit the "rush to the poles" close to solar maximum, when the solar polar magnetic field reverses polarity. In order to better understand the behavior of the "rush to the poles," we used cross-correlation analysis and wavelet transform methods for investigating the periodic characteristics and the phase relationship between two groups of the solar filaments at high latitudes observed during the period from 1919 March to 1989 December. The length of the solar cycle derived from the continuous wavelet transform is a function of latitude, but still shows a significant 11-yr cycle. The most significant periods of the solar filaments, respectively at higher latitudes than 50 degrees and 60 degrees, are 10.77 and 10.62 yr, using the wavelet transform method. From the cross-correlation analysis, the solar filaments at higher latitudes than 50 degrees have a lead of six months with respect to those at higher latitudes than 60 degrees. Different solar cycles exhibited different phase relationships between the two groups of solar filaments. The analysis of the cross-wavelet transform also indicates that the solar filaments at higher latitudes than 50 degrees lead those at higher latitudes than 60 degrees in the entire time interval. The relationship between the phase difference of the two groups of solar filaments and the intensity of solar activity is also discussed. What is more, the poleward shifting speeds are estimated. |
| Databáze: | OpenAIRE |
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