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The solar inner corona is a region that plays a critical role in energizingthe solar wind and propelling it to supersonic and supra-Alfvenic velocities.Despite its importance, this region remains poorly understood because of beingleast explored due to observational limitations. The coronal radio soundingtechnique in this context becomes useful as it helps in providing informationin parts of this least explored region. To shed light on the dynamics of thesolar wind in the inner corona, we conducted a study using data obtained fromcoronal radio-sounding experiments carried out by the Akatsuki spacecraftduring the 2021 Venus-solar conjunction event. By analyzing X-band radiosignals recorded at two ground stations (IDSN in Bangalore and UDSC in Japan),we investigated plasma turbulence characteristics and estimated flow speedmeasurements based on isotropic quasi-static turbulence models. Our analysisrevealed that the speed of the solar wind in the inner corona (at heliocentricdistances from 5 to 13 solar radii), ranging from 220-550 km/sec, was higherthan the expected average flow speeds in this region. By integrating ourradio-sounding results with EUV images of the solar disk, we gained a uniqueperspective on the properties and energization of high-velocity plasma streamsoriginating from coronal holes. We tracked the evolution of fast solar windstreams emanating from an extended coronal hole as they propagated toincreasing heliocentric distances. Our study provides unique insights into theleast-explored inner coronal region by corroborating radio sounding resultswith EUV observations of the corona.

Turbulence dynamics and flow speeds in the inner solar corona: Results from radio-sounding experiments by the Akatsuki spacecraft