Latitudinal Distribution of Photospheric Magnetic Fields of Different Magnitudes
| Autor: | M. I. Tyasto, D. G. Baranov, E. S. Vernova |
|---|---|
| Rok vydání: | 2016 |
| Předmět: |
Physics
Sunspot Solar observatory 010504 meteorology & atmospheric sciences Field (physics) FOS: Physical sciences Coronal hole Astronomy and Astrophysics Astrophysics 01 natural sciences Magnetic field Dipole Distribution (mathematics) Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Physics::Space Physics 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Polar Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences |
| Zdroj: | Solar Physics. 291:741-750 |
| ISSN: | 1573-093X 0038-0938 |
| DOI: | 10.1007/s11207-016-0862-9 |
| Popis: | Photospheric magnetic fields are studied using synoptic maps from 1976 to 2003 produced at the National Solar Observatory, Kitt Peak (NSO/KP). Synoptic maps were averaged over the time interval of nearly three solar cycles (Solar Cycles 21-23). The change in the latitudinal distribution was considered for the following groups of magnetic field values: B = 0-5 G, B = 5-15 G, B = 15-50 G, and B>50 G. Magnetic fields in each of the above groups have common latitudinal distribution features, while for different field groups these features are significantly different. Each of the groups is closely related to a certain manifestation of solar activity. Strong magnetic fields are connected with two types of solar activity: active regions (magnetic fields B>15 G)that are related to sunspot zones, and polar faculae (magnetic fields 50 G > B > 15 G) that occupy latitudes around 65$^\circ$-75$^\circ$. Fields from 5 to 15 G occupy the polar regions and are connected with polar coronal holes (the global solar dipole). Fields of B 11 pages, 8 figures |
| Databáze: | OpenAIRE |
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