On the Quasi-linear Transport of Magnetic Field Lines

Details On the Quasi-linear Transport of Magnetic Field Lines On the Quasi-linear Transport of Magnetic Field Lines

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...525..524r&link_type=abstract

The Astrophysical Journal, Volume 525, Issue 1, pp. 524-532.

Astronomy and Astrophysics

Astronomy

21

Chaos, Diffusion, Interplanetary Medium, Magnetic Fields, Sun: Solar Wind, Turbulence

Scientific paper

Under the assumption that a finite correlation length, Lc, exists and is much smaller than the size of the system, the quasi-linear theory for weak magnetic turbulence predicts, beyond Lc, a linear spreading of the magnetic field lines, <Δr2⊥>, as a function of the elapsed distance z along the main magnetic field, B0. When the power spectrum of the turbulence flattens at low wavenumbers, as was deduced from early observations of the interplanetary turbulence and is expected for an isotropic turbulence, the correlation length can be estimated as the Alfvén speed times the reciprocal of the upper frequency in the flat spectrum. However, more recent measurements of the solar wind magnetic power spectrum indicate a more complex spectrum at low frequencies. The field-lines' spreading in the quasi-linear regime of turbulence is derived here as a function of z for a general power spectrum. The transport exponent α, defined by <Δr2⊥>~zα, can be deduced from the projection along B0 of the spectrum. Normal (α=1), supradiffusive (α>1), and subdiffusive (α<1) predictions are made, depending on the shape at low wavenumbers assumed for the projected spectrum, which is related to the anisotropy and |k|-form of the three-dimensional spectrum.

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