Numerical simulation of Alfvénic turbulence in the solar wind

Details Numerical simulation of Alfvénic turbulence in the solar wind Numerical simulation of Alfvénic turbulence in the solar wind

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..535g&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 535-538 (1999).

Physics

Solar Wind Plasma, Sources Of Solar Wind, Magnetohydrodynamics And Plasmas

Scientific paper

We demonstrate that in an expanding volume, velocity shears and pressure-balanced flux tubes reduce the Alfvénicity of parallel propagating wave packets, as had been found previously in Cartesian geometry. The resulting power spectra have an inertial range spectral index of approximately 5/3. These three-dimensional spherically expanding simulations can include velocity shears separating fast and slow flows, pressure-balanced flux tubes, and a central current sheet. Two-dimensional spectra constructed in the r-θ plane resemble closely those resulting from similar initial conditions in Cartesian geometry.

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