Magnetic fluctuation spectrum in the inner solar wind

Details Magnetic fluctuation spectrum in the inner solar wind Magnetic fluctuation spectrum in the inner solar wind

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sf2a.conf..537g&link_type=abstract

SF2A-2006: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: D. Barret, F. Casoli, G.

Astronomy and Astrophysics

Astrophysics

Scientific paper

Waves and turbulence are ubiquitous in the inner solar wind. Whereas Alfvén waves and Kolmogorov-type energy spectra are found at low frequencies, whistler waves and steeper magnetic fluctuation power law spectra are detected at frequencies higher than a fraction of hertz (at 1 AU). This multi-scale turbulence behavior may be investigated in the framework of 3D Hall MHD. In that context, I have developed a wave turbulence analysis which shows that the steepening of magnetic spectra may be attributed to dispersive nonlinear processes rather than pure dissipation as often stated.

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