Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence

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
Hauptverfasser: 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.
Format: Artikel
Sprache:eng
Schlagworte:
Astronomy
Astrophysics
Coronal lines
Coronal loops
Heat
Magnetic fields
Observational research
Photospheres
Solar observatories
Solar prominences
Space based observatories
Sun
Sunspots
Wave propagation
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Beschreibung
Zusammenfassung: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.
ISSN:0036-8075
1095-9203
DOI:10.1126/science.1145447