Velocity Power Spectra from Cross-field Turbulence in the Proton Kinetic Regime

Details Velocity Power Spectra from Cross-field Turbulence in the Proton Kinetic Regime Velocity Power Spectra from Cross-field Turbulence in the Proton Kinetic Regime

Mar 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...747...19v&link_type=abstract

The Astrophysical Journal, Volume 747, Issue 1, article id. 19 (2012).

Astronomy and Astrophysics

Astronomy

Magnetohydrodynamics: Mhd, Solar Wind, Turbulence

Scientific paper

Numerical hybrid simulations with particle protons and fluid electrons are conducted for turbulent fluctuations with spatial variations in a plane perpendicular to the background magnetic field. In the turbulent phase, the proton bulk velocity spectrum has a dissipation range starting at a smaller wavenumber than the magnetic spectrum dissipation range. The steepened portion of the proton bulk velocity spectrum is constrained to a smaller wavenumber with an increasing ratio of background proton plasma to magnetic pressure β p . The form of the magnetic spectrum does not depend on β p . The collisionless proton and fluctuation interaction which heats protons mainly across the magnetic field is deemed to be the result of a viscous-like interaction based, in part, on the dependence of the velocity spectrum on β p .

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