Kinetic turbulence in relativistic plasma: from thermal bath to non-thermal continuum

Vladimir Zhdankin; Gregory R. Werner; Dmitri A. Uzdensky; Mitchell C. Begelman

doi:10.1103/PhysRevLett.118.055103

paper

Kinetic turbulence in relativistic plasma: from thermal bath to non-thermal continuum

arXiv:1609.04851 · doi:10.1103/PhysRevLett.118.055103

Abstract

We present results from particle-in-cell simulations of driven turbulence in magnetized, collisionless, and relativistic pair plasma. We find that fluctuations are consistent with the classical $k_{⊥}^{- 5/3}$ magnetic energy spectrum at fluid scales and a steeper $k_{⊥}^{- 4}$ spectrum at sub-Larmor scales, where $k_{⊥}$ is the wavevector perpendicular to the mean field. We demonstrate the development of a non-thermal, power-law particle energy distribution, $f (E) \sim E^{- α}$ , with index $α$ that decreases with increasing magnetization and increases with increasing system size (relative to the characteristic Larmor radius). Our simulations indicate that turbulence can be a viable source of energetic particles in high-energy astrophysical systems, such as pulsar wind nebulae, if scalings asymptotically become insensitive to the system size.

arXiv comment6 pages, 4 figures, to appear in PRL

Kinetic turbulence in relativistic plasma: from thermal bath to non-thermal continuum

Abstract

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