Vertical propagation of waves in the solar atmosphere. I. Observations of phase delays
Vertical propagation of waves in the solar atmosphere. I. Observations of phase delays
复制标题
波在太阳大气中的垂直传播。
DOI：
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发表时间：
1979
期刊：
影响因子：
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通讯作者：
E. Chipman
中科院分区：
文献类型：
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作者：
B. Lites;E. Chipman
萨克拉门托峰天文台塔真空望远镜，中阶梯光栅摄谱仪和二极管阵列被用来同时测量速度和强度在三个光谱线和连续。根据我们的贡献函数计算，这些波长是在从低光球层到色球层的高度上形成的。在0- 11.1mHz范围内，确定了不同高度之间强度和速度振荡的相速度，以及在一个高度上强度和速度之间的相位关系，作为频率的函数。振荡被发现主要是渐逝的频率小于4兆赫的性质，并在更高的频率向上传播，与接近声速在约6兆赫的相速度。我们计算了向上的机械通量在两个大气高度的观测波的频率积分，我们表明，在色球层的传播功率集中在6 MHz，但仍然太小，加热覆盖的大气。
The Sacramento Peak Observatory Tower Vacuum Telescope, echelle spectrograph, and diode array were used to simultaneously measure velocities and intensities in three spectral lines and the continuum. According to our contribution function calculations, these wavelengths are formed at heights from the low photosphere to the chromosphere. The phase velocities of the intensity and velocity oscillations between the various heights, and the phase relations between intensity and velocity at one height were determined as a function of frequency in the range 0--11.1 mHz. The oscillations are found to be predominantly evanescent in nature for frequencies less than 4 mHz and propagating upward at higher frequencies, with phase velocities approaching the sound speed at approximately 6 mHz. We calculated the upward mechanical flux in the observed waves at two atmospheric heights by an integration in frequency, and we show that in the chromosphere the propagated power is centered at 6 MHz but is still much too small to heat the overlying atmosphere.