Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence

Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence
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DOI：
10.1126/science.1145447
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发表时间：
2007-12
期刊：
Science
影响因子：
56.9
通讯作者：
T. J. Okamoto;S. Tsuneta;T. E. Berger;K. Ichimoto;Y. Katsukawa;B. Lites;S. Nagata;K. Shibata
T. J. Okamoto;S. Tsuneta;T. E. Berger;K. Ichimoto;Y. Katsukawa;B. Lites;S. Nagata;K. Shibata
中科院分区：
综合性期刊1区
文献类型：
--
作者：
T. J. Okamoto;S. Tsuneta;T. E. Berger;K. Ichimoto;Y. Katsukawa;B. Lites;S. Nagata;K. Shibata

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日珥是由周围 106 开尔文日冕等离子体支撑的 104 开尔文冷等离子体云，其机制尚未确定。日之出的观测显示，精细尺度的线状结构在天空平面上以几分钟的周期振荡。我们认为这些代表了在日冕磁场线上传播的阿尔文波，并且它们可能在加热日冕方面发挥了作用。
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.