Solar activity II: Sunspots and pores
Sunspots and pores appear as a consequence of interactions between strong magnetic fields and moving plasma. A wide variety of small‐scale features, presumably of convective origin, are observed in photospheric layers of sunspots and pores: Umbral dots, light bridges, penumbral filaments, and penumb...
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| Published in: | Astronomische Nachrichten Vol. 324; no. 4; pp. 369 - 373 |
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| Main Author: | |
| Format: | Journal Article |
| Language: | English |
| Published: |
Berlin
WILEY-VCH Verlag
01-06-2003
WILEY‐VCH Verlag |
| Subjects: | |
| Online Access: | Get full text |
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| Summary: | Sunspots and pores appear as a consequence of interactions between strong magnetic fields and moving plasma. A wide variety of small‐scale features, presumably of convective origin, are observed in photospheric layers of sunspots and pores: Umbral dots, light bridges, penumbral filaments, and penumbral grains. Each type of features has specific morphological, photometric, spectral, and kinematic characteristics. Spots and pores modify velocity fields in adjacent photosphere and sub‐photospheric layers. Recent high‐resolution spectral, broad‐band, and helioseismic observations of the structure, dynamics, and magnetic fields of sunspots and pores, together with theoretical interpretations, are discussed in this review. |
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| Bibliography: | istex:18E990550328C53CE4B064E3C056BA22EA5922D1 ark:/67375/WNG-6C4R1PN5-K ArticleID:ASNA200310132 |
| ISSN: | 0004-6337 1521-3994 |
| DOI: | 10.1002/asna.200310132 |