Fig. 9.

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Composite spectrum of all available radio observations from the Earth vantage point (9 GHz–10 kHz) together with STIX non-thermal (25–50 keV) count rates (top panel) and the in situ electrons observed at Solar Orbiter (bottom panel). The Solar Orbiter electron observations from the sunward telescope are time-shifted using the nominal path length and corrected for the travel time of light to make them comparable to the radio observations. The inferred injection time of the low-energy (high-energy) electrons are marked with the dotted (dot-dashed) line. With the pink (blue) shaded area we mark the release times using path length values larger than the nominal. For ∼0.85 AU, the earliest release of the low-energy electrons is near the start of the first group of type III radio burst. The dashed line indicates the peak of the electron intensity for the ∼55 keV electron channel.
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