Volume 661, May 2022
|Number of page(s)||8|
|Section||The Sun and the Heliosphere|
|Published online||13 May 2022|
The incompressible energy cascade rate in anisotropic solar wind turbulence
Instituto de Astronomía y Física del Espacio, CONICET-UBA, Ciudad Universitaria, 1428 Buenos Aires, Argentina
2 Departamento de Física, Facultad de Ciencias Exactas y Naturales, UBA, Ciudad Universitaria, 1428 Buenos Aires, Argentina
3 Laboratoire de Physique des Plasmas, École Polytechnique, CNRS, Sorbonne University, Observatoire de Paris, Univ. Paris-Saclay, 91128 Palaiseau Cedex, France
4 School of Electronic and Information, Wuhan University, Wuhan, PR China
5 Institut Universitaire de France, Paris, France
Accepted: 29 March 2022
Context. The presence of a magnetic guide field induces several types of anisotropy in solar wind turbulence. The energy cascade rate between scales in the inertial range depends strongly on the direction of this magnetic guide field, splitting the energy cascade according to the parallel and perpendicular directions with respect to magnetic guide field.
Aims. Using more than two years of Parker Solar Probe (PSP) observations, the isotropy and anisotropy energy cascade rates are investigated. The variance and normalized fluctuation ratios, the kinetic and magnetic energies, and the normalized cross-helicity and residual energy are studied. The connection between the heliocentric distance, the local temperature of the plasma, and the energy cascade components is made.
Methods. Using exact relations for fully developed incompressible magnetohydrodynamic (MHD) turbulence, the incompressible energy cascade rate is computed. In particular, using the isotropy and 2D and slab assumptions, the isotropic, perpendicular, and parallel energy cascade rate components are estimated.
Results. The variance anisotropy ratios, for both velocity and magnetic fields, do not exhibit a dependence with respect to the heliocentric distance r between 0.2 and 0.8 au. While the velocity normalized fluctuation ratio shows a dependence with r, the magnetic normalized fluctuation ratio does not. A strong correlation between the isotropic and anisotropic energy cascade rates and the temperature is found. A clear dominance of the perpendicular cascades over the parallel cascades as PSP approaches the Sun is observed. A dominant 2D cascade and/or geometry over the slab component in slow solar wind turbulence in the largest MHD scales is observed.
Key words: turbulence / magnetohydrodynamics (MHD) / plasmas
© ESO 2022
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