A comparison of the oscillations in sunspot umbrae, penumbrae, and the surrounding photosphere
A comparison of the oscillations in sunspot umbrae, penumbrae, and the surrounding photosphere
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太阳黑子本影、半影和周围光球层振荡的比较
DOI：
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发表时间：
1987
期刊：
影响因子：
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通讯作者：
E. Wiehr
中科院分区：
文献类型：
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作者：
H. Balthasar;G. Küveler;E. Wiehr
已在多个太阳黑子中用 100 x 100 二极管阵列观测到非分裂 Fei 7090 Å 线的时间序列，对应于 48 角秒乘以 1.39 Å。沿着一个固定狭缝位置的多普勒运动的空间行为已经被研究为时间的函数。先前的结果证实，五分钟范围内的功率从光球层到本影逐渐减小，然而，测量到的值仍然远高于噪声水平。关于半影，功率往往在径向水平场的视线分量应该最大的位置处表现出最大值。这表明振荡速度的方向可能会受到磁场或安歇德流的影响。在 3 分钟范围内没有发现明显的功率。在一个点的本影边缘的一小块斑块中可能会看到一个例外。
Time series of the nonsplit Fei 7090 Å line have been observed in several sunspots with a 100 x 100 diode array corresponding to 48 arc sec times 1.39 Å. The spatial behaviour of Doppler motions along one fixed slit position has been studied as a function of time. Former results are confirmed, that the power in the five minute range decreases from the photosphere to the umbra, where, however, values still well above the noise level are measured. Regarding the penumbra, the power tends to exhibit a maximum at locations where the line-of-sight component of a radial horizontal field should be maximal. This indicates that the direction of the oscillatory velocities might be influenced by the magnetic field or the Evershed flow. No significant power is found in the 3 min range. An exception might be seen in a small patch at the limb of the umbra of one spot.