Periodic change of polarity of photospheric magnetic field
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arXiv
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| Autori principali: | , , |
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| Natura: | Preprint |
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2025
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| _version_ | 1866909677422379008 |
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| author | Vernova, Elena Tyasto, Marta Baranov, Dmitrii |
| author_facet | Vernova, Elena Tyasto, Marta Baranov, Dmitrii |
| contents | The work is devoted to the study of periodic structures in the magnetic field of the photosphere. The polarity of the Sun's magnetic fields shows cyclicity with periods of 1-3 years, which is possibly due to quasi-biennial variations that are found in various parameters of solar activity, interplanetary space, and in cosmic rays. In this work, variations in weak magnetic fields of the photosphere were investigated, which required the use of special data processing methods. Synoptic maps of the photospheric magnetic field for the period 1978-2016 (NSO Kitt Peak) were used. To highlight the contribution of weak magnetic fields, the saturation threshold for synoptic maps was set at 5 G. Based on thus transformed synoptic maps, a time-latitude diagram was constructed. For the selected latitude intervals, smoothing, trend removal and Fast Fourier Transform (FFT) were performed. In the time-latitude diagram, 6 spatiotemporal regions with distinct cyclic structure were observed during 4 solar cycles (21-24). The periods ranged from 0.5 to 4 years with a maximum at 1.2 years. The amplitude of ripples is significantly higher for those intervals in which the polar field had positive sign. This effect confirms the connection of ripples variations with the polarity of the 22-year magnetic cycle. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_04912 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Periodic change of polarity of photospheric magnetic field Vernova, Elena Tyasto, Marta Baranov, Dmitrii Solar and Stellar Astrophysics The work is devoted to the study of periodic structures in the magnetic field of the photosphere. The polarity of the Sun's magnetic fields shows cyclicity with periods of 1-3 years, which is possibly due to quasi-biennial variations that are found in various parameters of solar activity, interplanetary space, and in cosmic rays. In this work, variations in weak magnetic fields of the photosphere were investigated, which required the use of special data processing methods. Synoptic maps of the photospheric magnetic field for the period 1978-2016 (NSO Kitt Peak) were used. To highlight the contribution of weak magnetic fields, the saturation threshold for synoptic maps was set at 5 G. Based on thus transformed synoptic maps, a time-latitude diagram was constructed. For the selected latitude intervals, smoothing, trend removal and Fast Fourier Transform (FFT) were performed. In the time-latitude diagram, 6 spatiotemporal regions with distinct cyclic structure were observed during 4 solar cycles (21-24). The periods ranged from 0.5 to 4 years with a maximum at 1.2 years. The amplitude of ripples is significantly higher for those intervals in which the polar field had positive sign. This effect confirms the connection of ripples variations with the polarity of the 22-year magnetic cycle. |
| title | Periodic change of polarity of photospheric magnetic field |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.04912 |