The reversal of the Sun’s magnetic field in cycle 24
Analysis of synoptic data from the Vector Spectromagnetograph (VSM) of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) and the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope facility shows that the reversals of solar polar magnetic fields exhibit elements o...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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INFRA-M
2016-03-01
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| Series: | Solar-Terrestrial Physics |
| Subjects: | |
| Online Access: | https://naukaru.ru/ru/nauka/article/12007/view |
| _version_ | 1828453759055822848 |
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| author | Mordvinov A.V. Pevtsov A.A. Bertello L. Petrie G.J.D. |
| author_facet | Mordvinov A.V. Pevtsov A.A. Bertello L. Petrie G.J.D. |
| author_sort | Mordvinov A.V. |
| collection | DOAJ |
| description | Analysis of synoptic data from the Vector Spectromagnetograph (VSM) of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) and the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope facility shows that the reversals of solar polar magnetic fields exhibit elements of a stochastic process, which may include the development of specific patterns of emerging magnetic flux, and the asymmetry in activity between Northern and Southern hemispheres. The presence of such irregularities makes the modeling and prediction of polar field reversals extremely hard if possible. In a classical model of solar activity cycle, the unipolar magnetic regions (UMRs) of predominantly following polarity fields are transported polewards due to meridional flows and diffusion. The UMRs gradually cancel out the polar magnetic field of the previous cycle, and rebuild the polar field of opposite polarity setting the stage for the next cycle. We show, however, that this deterministic picture can be easily altered by the developing of a strong center of activity, or by the emergence of an extremely large active region, or by a ‘strategically placed’ coronal hole. We demonstrate that the activity occurring during the current cycle 24 may be the result of this randomness in the evolution of the solar surface magnetic field. |
| first_indexed | 2024-12-11T00:12:21Z |
| format | Article |
| id | doaj.art-3e330e157bb54c129d5be100d102e2ae |
| institution | Directory Open Access Journal |
| issn | 2500-0535 |
| language | English |
| last_indexed | 2024-12-11T00:12:21Z |
| publishDate | 2016-03-01 |
| publisher | INFRA-M |
| record_format | Article |
| series | Solar-Terrestrial Physics |
| spelling | doaj.art-3e330e157bb54c129d5be100d102e2ae2022-12-22T01:28:06ZengINFRA-MSolar-Terrestrial Physics2500-05352016-03-012131810.12737/19856The reversal of the Sun’s magnetic field in cycle 24Mordvinov A.V.0Pevtsov A.A.1Bertello L.2Petrie G.J.D.3Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, RussiaNational Solar Observatory, Sunspot, New Mexico 88349, USANational Solar Observatory, Tucson, Arizona, USANational Solar Observatory, Tucson, Arizona, USAAnalysis of synoptic data from the Vector Spectromagnetograph (VSM) of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) and the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope facility shows that the reversals of solar polar magnetic fields exhibit elements of a stochastic process, which may include the development of specific patterns of emerging magnetic flux, and the asymmetry in activity between Northern and Southern hemispheres. The presence of such irregularities makes the modeling and prediction of polar field reversals extremely hard if possible. In a classical model of solar activity cycle, the unipolar magnetic regions (UMRs) of predominantly following polarity fields are transported polewards due to meridional flows and diffusion. The UMRs gradually cancel out the polar magnetic field of the previous cycle, and rebuild the polar field of opposite polarity setting the stage for the next cycle. We show, however, that this deterministic picture can be easily altered by the developing of a strong center of activity, or by the emergence of an extremely large active region, or by a ‘strategically placed’ coronal hole. We demonstrate that the activity occurring during the current cycle 24 may be the result of this randomness in the evolution of the solar surface magnetic field.https://naukaru.ru/ru/nauka/article/12007/viewsolar cyclesunspot activitymagnetic fieldscoronal holes |
| spellingShingle | Mordvinov A.V. Pevtsov A.A. Bertello L. Petrie G.J.D. The reversal of the Sun’s magnetic field in cycle 24 Solar-Terrestrial Physics solar cycle sunspot activity magnetic fields coronal holes |
| title | The reversal of the Sun’s magnetic field in cycle 24 |
| title_full | The reversal of the Sun’s magnetic field in cycle 24 |
| title_fullStr | The reversal of the Sun’s magnetic field in cycle 24 |
| title_full_unstemmed | The reversal of the Sun’s magnetic field in cycle 24 |
| title_short | The reversal of the Sun’s magnetic field in cycle 24 |
| title_sort | reversal of the sun s magnetic field in cycle 24 |
| topic | solar cycle sunspot activity magnetic fields coronal holes |
| url | https://naukaru.ru/ru/nauka/article/12007/view |
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