Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence
Solar prominences are cool 10⁴ kelvin plasma clouds supported in the surrounding 10⁶ kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these repr...
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| Veröffentlicht in: | Science (American Association for the Advancement of Science) 2007-12, Vol.318 (5856), p.1577-1580 |
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| creator | Okamoto, T. J. Tsuneta, S. Berger, T. E. Ichimoto, K. Katsukawa, Y. Lites, B. W. Nagata, S. Shibata, K. Shimizu, T. Shine, R. A. Suematsu, Y. Tarbell, T. D. Title, A. M. |
| description | Solar prominences are cool 10⁴ kelvin plasma clouds supported in the surrounding 10⁶ kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role in heating the corona. |
| doi_str_mv | 10.1126/science.1145447 |
| format | Article |
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| source | American Association for the Advancement of Science; Jstor Complete Legacy |
| subjects | Astronomy Astrophysics Coronal lines Coronal loops Heat Magnetic fields Observational research Photospheres Solar observatories Solar prominences Space based observatories Sun Sunspots Wave propagation |
| title | Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence |
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