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Observation and Modeling of the Solar Wind Turbulence Evolution in the Sub-Mercury Inner Heliosphere

2022; IOP Publishing; Volume: 938; Issue: 2 Linguagem: Inglês

10.3847/2041-8213/ac9624

2041-8213

Daniele Telloni, L. Adhikari, G. P. Zank, Lina Hadid, Beatriz Sánchez–Cano, L. Sorriso‐Valvo, Lingling Zhao, O. Panasenco, Chen Shi, M. Velli, Roberto Susino, Daniel Verscharen, A. Milillo, Tommaso Alberti, Yasuhito Narita, Andrea Verdini, C. Grimani, R. Bruno, R. D’Amicis, Denise Perrone, R. Marino, Francesco Carbone, F. Califano, F. Malara, J. E. Stawarz, R. Laker, Alessandro Liberatore, S. D. Bale, J. C. Kasper, Daniel Heyner, Thierry Dudok de Wit, K. Goetz, P. Harvey, R. J. MacDowall, D. Malaspina, M. Pulupa, A. W. Case, K. E. Korreck, D. E. Larson, R. Livi, M. L. Stevens, P. L. Whittlesey, Hans‐Ulrich Auster, Ingo Richter,

Geomagnetism and Paleomagnetism Studies

Abstract This letter exploits the radial alignment between the Parker Solar Probe and BepiColombo in late 2022 February, when both spacecraft were within Mercury’s orbit. This allows the study of the turbulent evolution, namely, the change in spectral and intermittency properties, of the same plasma parcel during its expansion from 0.11 to 0.33 au, a still unexplored region. The observational analysis of the solar wind turbulent features at the two different evolution stages is complemented by a theoretical description based on the turbulence transport model equations for nearly incompressible magnetohydrodynamics. The results provide strong evidence that the solar wind turbulence already undergoes significant evolution at distances less than 0.3 au from the Sun, which can be satisfactorily explained as due to evolving slab fluctuations. This work represents a step forward in understanding the processes that control the transition from weak to strong turbulence in the solar wind and in properly modeling the heliosphere.