Common Origin of Kinetic Scale Turbulence and the Electron Halo in the Solar Wind -- Connection to Nanoflares

@article{Che2016CommonOO,
  title={Common Origin of Kinetic Scale Turbulence and the Electron Halo in the Solar Wind -- Connection to Nanoflares},
  author={Haihong Che},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2016}
}
  • H. Che
  • Published 2 March 2016
  • Physics
  • arXiv: Solar and Stellar Astrophysics
We summarize our recent studies on the origin of solar wind kinetic scale turbulence and electron halo in the electron velocity distribution function. Increasing observations of nanoflares and microscopic type III radio bursts strongly suggest that nanoflares and accelerated electron beams are common in the corona. Based on particle-in-cell simulations, we show that both the core-halo feature and kinetic scale turbulence observed in the solar wind can be produced by the nonlinear evolution of… 

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References

SHOWING 1-10 OF 60 REFERENCES

THE ORIGIN OF NON-MAXWELLIAN SOLAR WIND ELECTRON VELOCITY DISTRIBUTION FUNCTION: CONNECTION TO NANOFLARES IN THE SOLAR CORONA

The formation of the observed core-halo feature in the solar wind electron velocity distribution function is a long-time puzzle. In this Letter, based on the current knowledge of nanoflares, we show

ELECTRON TRANSPORT IN THE FAST SOLAR WIND

The electron velocity distribution function is studied in the extended solar corona above coronal holes (i.e., the inner part of the fast solar wind) from the highly collisional corona close to the

Kinetic Physics of the Solar Corona and Solar Wind

Kinetic plasma physics of the solar corona and solar wind are reviewed with emphasis on the theoretical understanding of the in situ measurements of solar wind particles and waves, as well as on the

Bidirectional energy cascades and the origin of kinetic Alfvénic and whistler turbulence in the solar wind.

Using particle-in-cell simulations, this work explores how the free energy released by an electron two-stream instability drives Weibel-like electromagnetic waves that excite wave-wave interactions that evolve through inverse and forward magnetic energy cascades.

Electron Halo and Strahl Formation in the Solar Wind by Resonant Interaction with Whistler Waves

Observations of solar wind electron distribution functions (VDFs) reveal considerable deviations from a simple Maxwellian VDF. A thermal core and a suprathermal halo and antisunward, magnetic

IDENTIFICATION OF KINETIC ALFVÉN WAVE TURBULENCE IN THE SOLAR WIND

The nature of small-scale turbulent fluctuations in the solar wind is investigated using a comparison of Cluster magnetic and electric field measurements to predictions arising from models consisting

Kinetic Models for Whistler Wave Scattering of Electrons in the Solar Corona and Wind

Kinetic models are necessary to describe the physical processes associated with non-Maxwellian velocity distribution functions (VDFs) of electrons or ions in the solar corona and wind. It is shown

ON THE COMPETITION BETWEEN RADIAL EXPANSION AND COULOMB COLLISIONS IN SHAPING THE ELECTRON VELOCITY DISTRIBUTION FUNCTION: KINETIC SIMULATIONS

We present numerical simulations of the solar wind using a fully kinetic model which takes into account the effects of particle's binary collisions in a quasi-neutral plasma in spherical expansion.

Helios: Evolution of Distribution Functions 0.3–1 AU

The radial evolution of the velocity distribution functions of the protons, electrons and ions, as they were measured during the Helios mission in the solar wind between 0.3 and 1.0 AU, is discussed

Evidence of a cascade and dissipation of solar-wind turbulence at the electron gyroscale.

The first direct determination of the dissipation range of magnetofluid turbulence in the solar wind at the electron scales is reported and a remarkable agreement with theoretical predictions of a quasi-two-dimensional cascade into Kinetic Alfvén Waves (KAW).
...