Dissipation Wavenumbers for Turbulence in Electron-Positron Plasmas

Details Dissipation Wavenumbers for Turbulence in Electron-Positron Plasmas Dissipation Wavenumbers for Turbulence in Electron-Positron Plasmas

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...701.1695g&link_type=abstract

The Astrophysical Journal, Volume 701, Issue 2, pp. 1695-1700 (2009).

Astronomy and Astrophysics

Astronomy

1

Plasmas, Turbulence

Scientific paper

Many astrophysical systems involve turbulent electron-positron plasmas. Linear kinetic theory of electromagnetic fluctuations in homogeneous, magnetized, collisionless, non-relativistic electron-positron plasmas predicts that two lightly damped modes propagate at relatively long wavelengths: an Alfvén-like mode with dispersion ω_r = k_{∥} \tilde{v}_A and a magnetosonic-like mode with dispersion ω_r ≃ k \tilde{v}_A if β e Lt 1. Here, \tilde{v}_A is the Alfvén speed in an electron-positron plasma and par refers to the direction parallel to the background magnetic field B o . The dissipation wavenumber kd is defined as the value of k at which the damping rate equals the rate of energy transfer by the turbulent cascade. Using linear theory and a basic turbulent cascade model, kd is predicted for turbulence at propagation quasi parallel to B o , for quasi-perpendicular magnetosonic-like turbulence, and for quasi-perpendicular Alfvén-like turbulence. In the latter case, the model predicts that an increase in the turbulent energy should correspond to an increase in kd . The assumptions and predictions of the model may be tested by particle-in-cell simulations.

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