D-Region Electron-Density Profiles during Auroras
D-Region Electron-Density Profiles during Auroras
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极光期间的 D 区电子密度分布
DOI：
10.1029/jz069i013p02857
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发表时间：
1964
期刊：
影响因子：
--
通讯作者：
R. Parthasarathy
中科院分区：
文献类型：
--
作者：
G. Lerfald;C. Little;R. Parthasarathy
这封信的目的是简要描述在阿拉斯加大学极光吸收事件期间获得的多频宇宙噪声吸收数据分析的初步结果。
单频riometer数据没有给出关于电离导致吸收发生的高度的信息。我们已经证明，然而[Parthasarathy等人，1963年]，宇宙噪声吸收数据采取广泛的间隔频率可以用来获得'最佳'电子密度分布在高度范围约30至75公里。基本上，该方法取决于以下事实：在不同频率上观察到的吸收比率是吸收区域中的电子碰撞频率v与角射频ω的比率的函数，因此随着吸收层的高度而变化。对于v/ω 1（大高度），观察到吸收的标准f−2依赖性;当v/ω增加到大值时，指数减小到零（即，低高度）。
The purpose of this letter is to describe briefly the preliminary results of an analysis of multifrequency cosmic noise absorption data taken during auroral absorption events at College, Alaska.
Single-frequency riometer data give no information as to the height at which the ionization causing the absorption occurs. We have shown, however [Parthasarathy et al., 1963], that cosmic noise absorption data taken on widely spaced frequencies can be used to derive ‘bestfit’ electron density profiles over the height range of approximately 30 to 75 km. Basically, the method depends on the fact that the ratio of absorption observed on different frequencies is a function of the ratio of the electron collision frequency v in the absorbing region to the angular radio frequency ω and therefore varies with the height of the absorbing layer. For v/ω≪1 (great heights) the standard f−2 dependence of the absorption is observed; the exponent decreases to zero as v/ω is increased to large values (i.e., for low heights).