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The reflection heights were determined from nearby ionospheric sounders.
The reflection heights were determined by two independent methods.
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 are estimated using the IRI 2012 model (Bilitza et al. 2014).
We recommend using the best possible practical height resolution and utilizing the calculated total reflection heights to omit contaminated data.
The calculations based on the sin correction show the lowering of reflection heights by ~1 2 km.
Similar(37)
First, as follows from the nature of spread F, the reflection height is of a random character, and the signal reflects from many different small-scale irregularities.
The best agreement was found for the effective reflection height.
Here, h true is the true reflection height.
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.
The true reflection height was lower than the corresponding maximum height by approximately 40 km.
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