Fig. F.1.
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Simulated decay times (top) and rise times (bottom) as a function of the angular separation, and their associated errors. The observers are located at the heliocentric distance of 1 au at varying angles from the source. Fundamental emissions with a frequency of ∼250 kHz were assumed, as well as a level of scattering ε = 0.8 and a level of anisotropy α = 0.3.
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