Phenomenology of non-Alfvenic turbulence in a uniformly expanding medium

Details Phenomenology of non-Alfvenic turbulence in a uniformly expanding medium Phenomenology of non-Alfvenic turbulence in a uniformly expanding medium

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.confq..80m&link_type=abstract

Delaware Univ., International Solar Wind 8 Conference, p. 80

Other

Magnetohydrodynamic Turbulence, Magnetohydrodynamic Waves, Solar Wind, Interplanetary Medium, Homogeneous Turbulence, Turbulence Models, Plasma Turbulence, Kolmogorov Theory, Transport Properties, Anisotropy, Magnetic Fields, Kinetic Energy

Scientific paper

Transport and decay of magnetohydrodynamic (MHD) turbulence in a weakly inhomogeneous uniformly expanding medium involves a fairly complex formalism, even for the case where no spectral information is required. Here we argue that the phenomenology for decay simplifies greatly if: (1) the cross helicity (Alfvenicity) is small, (2) the dynamical influence of the large scale magnetic field is negligible either because of spectral anisotropy or because the expansion speed is much greater than the corresponding Alfven speed, and (3) the ratio of kinetic energy to magnetic energy for the fluctuations is either unity or some other constant. These conditions are acceptable as an approximation to solar wind turbulence in the outer heliosphere. In these circumstances a reasonable MHD energy-containing phenomenology is essentially that of locally homogeneous Kolmogoroff turbulence in a uniformly expanding medium. Analytical solutions for this model are presented for both undriven and driven cases.

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