HIGHLIGHTS
SUMMARY
Solar wind in situ observations show that the magnetic_field spectrum follows a power law at large MHD scales, with a scaling exponent ranging between -3/2 and -5/3 depending on certain conditions, such as the SW speed and the heliocentric distance (Biskamp 2003; Chen et_al 2013, 2020). Both SW and magnetosheath measurements show that the magnetic_field spectrum breaks and steepens at ion scales. A uniform outof-plane guide field B0 is present and the turbulence is triggered by random phase isotropic magnetic_field and velocity perturbations with wavenumber k in the range 1 6 . . .
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