Compressible MHD Turbulence in the Slow Solar Wind: Energy Transfer Rate

Fouad Sahraoui (1) , Nahuel Andrés (1) , L. Z. Hadid (1) , Sébastien Galtier (1) , P. Dmitruk , P. D. Mininni

1 LPP - Laboratoire de Physique des Plasmas

The role of compressible fluctuations in the MHD turbulence is investigated using direct numerical simulations and in-situ spacecraft in the solar wind. A focus is put on verifying the exact third-order law derived for compressible isothermal turbulence by Banerjee and Galtier, 2013. The numerical simulations use a 3D compressible MHD code in the isothermal limit ( =1) with low sonic Mach numbers (Ms<1). The main goal is to evaluate the relative importance of the new flux and source terms involved in the derived law. Direct comparison with spacecraft observations from the Themis spacecraft in the fast and slow solar wind will be made.

Domaines: Physique des plasmas [physics.plasm-ph]; Astrophysique [astro-ph]

Fouad Sahraoui, Nahuel Andrés, L. Z. Hadid, Sébastien Galtier, P. Dmitruk, et al.. Compressible MHD Turbulence in the Slow Solar Wind: Energy Transfer Rate. American Geophysical Union, Fall General Assembly, Dec 2016, San Francisco, California, United States. 21, pp.SH21C-2538, 2016. ⟨hal-02861323⟩