Phase scintillation observation during coronal sounding experiments with NOZOMI spacecraft
Phase scintillation observation during coronal sounding experiments with NOZOMI spacecraft
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DOI：
10.1051/0004-6361:20042614
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发表时间：
2005-09
影响因子：
6.5
通讯作者：
T. Imamura;K. Noguchi;A. Nabatov;K. Oyama;Z. Yamamoto;M. Tokumaru
中科院分区：
文献类型：
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作者：
T. Imamura;K. Noguchi;A. Nabatov;K. Oyama;Z. Yamamoto;M. Tokumaru
2000年12月至2001年1月，利用日本的Nozomi航天器（行星-B）在太阳偏移距离12.8-36.9 RS处对日冕进行了无线电掩星观测。在S波段上行链路和X波段下行链路的双向模式下，获得了频率高达10 Hz的相位闪烁谱。光谱不能用单一的幂律来表示，特别是对于小的偏移距离。也就是说，在低频率（大尺度）的频谱显示的斜坡指示柯尔莫哥洛夫，局部平坦化发生从0.5 Hz（尺度为0.600 km）到0.3 Hz（尺度为0.100 km），和陡峭化再次发生在较高的频率。这种光谱的三分量性质是首次用单一方法观察到的，尽管光谱形状是可变的，三分量特征并不总是明显的。
Radio occultation observations of the solar corona at solar offset distances of 12.8-36.9 RS were performed from December of 2000 to January of 2001, using the Nozomi spacecraft (Planet-B) of Japan. Phase scintillation spectra up to the frequency of ∼10 Hz were obtained in two-way mode with S -band uplink and X-band downlink. The spectra cannot be represented by a single power law especially for small offset distances. That is, at low frequencies (large scales) the spectra show slopes indicative of Kolmogorov, a local flattening occurs from ∼0.5 Hz (scale ∼600 km) to ∼ 3H z (∼100 km), and a steepening occurs again at higher frequencies. This three-component nature of the spectrum was observed with a single method for the first time, although the spectral shape is variable and the three-component feature is not always evident.