A numerical model representing a 3D turbulent constant-magnitude magnetic field B is described. Assuming a form for two components of the vector potential, the third component is calculated such as to obtain a uniform intensity for B. Singular surfaces are always present in the solution, in the form of rotational discontinuities. Using a spectrum for derivatives of the given vector potential components that satisfies the critical-balance condition, an anisotropic spectrum for B is obtained, with a prevalence of perpendicular wavevectors k⊥ and a Kolmogorov power-law range with respect to k⊥. These features make the model suitable to represent magnetic turbulence in solar wind fast-speed streams.

Building up Solar-wind-like 3D Uniform-intensity Magnetic Fields

Valentini F.;Malara F.
;
Sorriso-Valvo L.;Bruno R.;Primavera L.
2019

Abstract

A numerical model representing a 3D turbulent constant-magnitude magnetic field B is described. Assuming a form for two components of the vector potential, the third component is calculated such as to obtain a uniform intensity for B. Singular surfaces are always present in the solution, in the form of rotational discontinuities. Using a spectrum for derivatives of the given vector potential components that satisfies the critical-balance condition, an anisotropic spectrum for B is obtained, with a prevalence of perpendicular wavevectors k⊥ and a Kolmogorov power-law range with respect to k⊥. These features make the model suitable to represent magnetic turbulence in solar wind fast-speed streams.
magnetic fields, solar wind, turbulence
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11770/295178
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