Helios 2 observations of solar wind turbulence decay in the inner heliosphere

¹ Swedish Institute of Space Physics (IRF), Ångström Laboratory, Lägerhyddsvägen 1, 75121 Uppsala, Sweden
e-mail: lucasorriso@gmail.com
² CNR, Istituto per la Scienza e la Tecnologia dei Plasmi, Via Amendola 122/D, 70126 Bari, Italy
³ Space and Plasma Physics, School of Electrical Engineering and Computer Science, KTH Royal Institute of Technology, Teknikringen 31, 11428 Stockholm, Sweden
⁴ Université de Lyon, CNRS, École Centrale de Lyon, INSA Lyon, Université Claude Bernard Lyon 1, Laboratoire de Mécanique des Fluides et d’Acoustique, UMR5509, 69134 Écully, France
⁵ Dipartimento di Scienze Fisiche e Chimiche, Università degli Studi dell’Aquila, Via Vetoio 42, 67100 Coppito, AQ, Italy
⁶ National Institute for Astrophysics (INAF) – Institute for Space Astrophysics and Planetology (IAPS), Via Fosso del Cavaliere, 100, 00133 Rome, Italy
⁷ National Institute for Astrophysics (INAF) – Astrophysical Observatory of Torino, Via Osservatorio 20, 10025 Pino Torinese, Italy

Received: 5 September 2022
Accepted: 17 February 2023

Abstract

Aims. A linear scaling of the mixed third-order moment of the magnetohydrodynamic (MHD) fluctuations is used to estimate the energy transfer rate of the turbulent cascade in the expanding solar wind.

Methods. In 1976, the Helios 2 spacecraft measured three samples of fast solar wind originating from the same coronal hole, at different distances from the Sun. Along with the adjacent slow solar wind streams, these intervals represent a unique database for studying the radial evolution of turbulence in samples of undisturbed solar wind. A set of direct numerical simulations of the MHD equations performed with the Lattice-Boltzmann code FLAME was also used for interpretation.

Results. We show that the turbulence energy transfer rate decays approximately as a power law of the distance and that both the amplitude and decay law correspond to the observed radial temperature profile in the fast wind case. Results from MHD numerical simulations of decaying MHD turbulence show a similar trend for the total dissipation, suggesting an interpretation of the observed dynamics in terms of decaying turbulence and that multi-spacecraft studies of the solar wind radial evolution may help clarify the nature of the evolution of the turbulent fluctuations in the ecliptic solar wind.