Kinetic Heating by Alfvén Waves in Magnetic Shears.

@article{Bacchini2021KineticHB,
  title={Kinetic Heating by Alfv{\'e}n Waves in Magnetic Shears.},
  author={Fabio Bacchini and Francesco Pucci and Francesco Malara and Giovanni Lapenta},
  journal={Physical review letters},
  year={2021},
  volume={128 2},
  pages={
          025101
        }
}
With first-principles kinetic simulations, we show that a large-scale Alfvén wave (AW) propagating in an inhomogeneous background decays into kinetic Alfvén waves (KAWs), triggering ion and electron energization. We demonstrate that the two species can access unequal amounts of the initial AW energy, experiencing differential heating. During the decay process, the electric field carried by KAWs produces non-Maxwellian features in the particle velocity distribution functions, in accordance with… 
1 Citations

Figures from this paper

Eulerian simulations of electrostatic waves in plasmas with a single sign of charge

An Eulerian, numerical simulation is used to model the launching of plasma waves in a non-neutral plasma that is confined in a Penning-Malmberg trap. The waves are launched by applying an oscillating

References

SHOWING 1-10 OF 65 REFERENCES

Kinetic Alfvén wave generation by velocity shear in collisionless plasmas

The evolution of a linearly polarized, long-wavelength Alfvén wave propagating in a collisionless magnetized plasma with a sheared parallel-directed velocity flow is here studied by means of

Coronal Heating by Magnetohydrodynamic Turbulence Driven by Reflected Low-Frequency Waves

A candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfvén waves, generated in the photosphere or chromosphere, with their

KINETIC ALFVÉN WAVE GENERATION BY LARGE-SCALE PHASE MIXING

One view of the solar wind turbulence is that the observed highly anisotropic fluctuations at spatial scales near the proton inertial length dp may be considered as kinetic Alfvén waves (KAWs). In

Alfvén Waves in the Solar Corona

An estimate of the energy carried by the waves that are spatially resolved indicates that they are too weak to heat the solar corona; however, unresolved Alfvén waves may carry sufficient energy.

Transition to kinetic turbulence at proton scales driven by large-amplitude kinetic Alfvén fluctuations

Space plasmas are dominated by the presence of large-amplitude waves, large-scale inhomogeneities, kinetic effects and turbulence. Beside the homogeneous turbulence, the generation of small scale

A Three Dimensional Magnetohydrodynamic Pulse in a Transversely Inhomogeneous Medium

Interaction of impulsively generated MHD waves with a one‐dimensional plasma inhomogeneity, transverse to the magnetic field, is considered in the three‐dimensional regime. Because of the transverse

Relativistic Alfvén Waves Entering Charge-starvation in the Magnetospheres of Neutron Stars

Instabilities in a neutron star can generate Alfvén waves in its magnetosphere. Propagation along the curved magnetic field lines strongly shears the wave, boosting its electric current j A. We

From Alfvén waves to kinetic Alfvén waves in an inhomogeneous equilibrium structure

Kinetic Alfvén waves are believed to primary form fluctuations in a hydromagnetic turbulence at scales of the order of the ion inertial length. We study a model where an initial Alfvén wave

Kinetic simulations of magnetized turbulence in astrophysical plasmas.

The first ab initio, fully electromagnetic, kinetic simulations of magnetized turbulence in a homogeneous, weakly collisional plasma at the scale of the ion Larmor radius (ion gyroscale) support the hypothesis that the frequencies of turbulent fluctuations in the solar wind remain well below the ion cyclotron frequency.

Alfvén Waves in the Solar Atmosphere

Alfvén waves are considered to be viable transporters of the non-thermal energy required to heat the Sun’s quiescent atmosphere. An abundance of recent observations, from state-of-the-art facilities,
...