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On many heating sessions simultaneous variations of the probing partial reflection signals in Vasil'sursk and backscattered signals in Observatory were observed at the height at 40 100 km below the reflection height of the pumping wave.
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The reflection height at low latitudes is higher than that at high latitudes.
ΔH′ = H′ − H′ p, where H′ is the quiescent-level ionospheric reflection height and H′ p is the reflection height during the solar flare peak.
Shvets and Hayakawa (1998) indicated that when the Sun,s activity decreases hence the reflection height increases.
Each panel in Fig. 4 presents the temporal variation of the reflection height with different harmonics.
The reflection heights at the time of totality during TSE are found to be less by 2 3 km as compared to the usual nighttime tweek reflection heights.
The reflection heights were determined by two independent methods.
The reflection heights were determined from nearby ionospheric sounders.
The reflection heights are estimated using the IRI 2012 model (Bilitza et al. 2014).
Whatever the actual height extent of the D region, or its subdivisions, in this review, we are focused on partial reflection of radar returns from the ionosphere in the region above 50 km, and below the total reflection height of the E region, for the purposes of investigating the neutral atmosphere.
In addition, close to, but below the total reflection height, group retardation means the reported heights (the virtual heights) are greater than the actual backscatter/partial reflection heights.
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