Formation of Solar Magnetic Flux Tubes with Kilogauss Field Strength Induced by Convective Instability
Formation of Solar Magnetic Flux Tubes with Kilogauss Field Strength Induced by Convective Instability
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DOI：
10.1086/588026
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发表时间：
2008-03
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通讯作者：
S. Nagata;S. Tsuneta;Y. Suematsu;K. Ichimoto;Y. Katsukawa;T. Shimizu;T. Yokoyama;T. Tarbell;B. Lites;R. Shine;T. Berger;A. Title;L. B. Bellot Rubio;D. Orozco Suárez
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作者：
S. Nagata;S. Tsuneta;Y. Suematsu;K. Ichimoto;Y. Katsukawa;T. Shimizu;T. Yokoyama;T. Tarbell;B. Lites;R. Shine;T. Berger;A. Title;L. B. Bellot Rubio;D. Orozco Suárez
对流不稳定性一直被用来解释具有kG场强的太阳光球通量管的形成。然而，地球大气层的湍流使地面观测者无法在亚弧秒尺度的通量管上进行精确的偏振测量来检验这一假设。在这里，我们讨论的观测证据，这种情况下的观测与太阳光学望远镜（SOT）日之出。在达到6 km s-1的瞬态下降流和增强到2 kG的场强之前，均分场强通量管的冷却。这些观测结果与理论预测非常吻合。
Convective instability has been a mechanism used to explain the formation of solar photospheric flux tubes with kG field strength. However, the turbulence of the Earth’s atmosphere has prevented ground-based observers from examining the hypothesis with precise polarimetric measurement on the subarcsecond scale flux tubes. Here we discuss observational evidence of this scenario based on observations with the Solar Optical Telescope (SOT) aboard Hinode. The cooling of an equipartition field strength flux tube precedes a transient downflow reaching 6 km s−1 and the intensification of the field strength to 2 kG. These observations agree very well with the theoretical predictions.