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Kinetic cascade beyond magnetohydrodynamics of solar wind turbulence in two-dimensional hybrid simulations
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10.1063/1.3682960
/content/aip/journal/pop/19/2/10.1063/1.3682960
http://aip.metastore.ingenta.com/content/aip/journal/pop/19/2/10.1063/1.3682960
View: Figures

Figures

Image of FIG. 1.
FIG. 1.

(Color online) Two-dimensional power spectral density of magnetic field fluctuations in arbitrary units for Run A. The background magnetic field is oriented along the kz -axis. The cascade of energy to higher wavenumbers occurs preferentially in the perpendicular direction.

Image of FIG. 2.
FIG. 2.

(Color online) Power spectral density of compressive fluctuations in the proton number density in arbitrary units for Run A. The spatial variation of the fluctuations occurs mainly perpendicular to the background magnetic field.

Image of FIG. 3.
FIG. 3.

(Color online) Power spectral density of fluctuations in the magnetic field and density at t = 500 along the perpendicular direction for Run A. A power law with spectral index − 5/3 is shown additionally, in order to estimate the slope of the spectrum.

Image of FIG. 4.
FIG. 4.

(Color online) Dispersion relation of magnetic field fluctuations parallel to the background magnetic field at t ≈ 500 for Run A. The overplotted lines indicate the F/W (upper line) and A/IC (lower line) wave branches calculated directly from the cold-plasma dispersion relation.

Image of FIG. 5.
FIG. 5.

(Color online) Dispersion relation of magnetic field fluctuations perpendicular to the background magnetic field at t ≈ 500 for Run A.

Image of FIG. 6.
FIG. 6.

(Color online) Dispersion relation of density fluctuations perpendicular to the background magnetic field at t ≈ 500 for Run A. The fluctuations coincide well with the magnetic fluctuations.

Image of FIG. 7.
FIG. 7.

(Color online) Correlation coefficient C between fluctuations of magnetic pressure and density depending on the averaging in space and time for Run A. A strong anti-correlation is found up to long averaging times, which correspond to low frequencies in the dispersion diagrams. This is an indication for the existence of PBSs. The units are given in the above introduced normalization.

Image of FIG. 8.
FIG. 8.

(Color online) Two-dimensional power spectral density of magnetic field fluctuations in arbitrary units for Run B. The background magnetic field is oriented along the kz -axis. Also in this case, the cascade is preferentially perpendicular.

Image of FIG. 9.
FIG. 9.

(Color online) Power spectral density of fluctuations in the magnetic field and density at t = 500 along the perpendicular direction for Run B.

Image of FIG. 10.
FIG. 10.

(Color online) Dispersion relation of magnetic field fluctuations parallel to the background magnetic field at t ≈ 500 for Run B. The overplotted lines indicate again the theoretical cold-plasma dispersion relations.

Image of FIG. 11.
FIG. 11.

(Color online) Dispersion relation of magnetic field fluctuations perpendicular to the background magnetic field at t ≈ 500 for Run B.

Image of FIG. 12.
FIG. 12.

(Color online) Temperature evolution of the protons for Run B. The temperatures versus time in the parallel and perpendicular directions with respect to the background magnetic field are shown. They are normalized to their initial values.

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/content/aip/journal/pop/19/2/10.1063/1.3682960
2012-02-16
2014-04-24
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Kinetic cascade beyond magnetohydrodynamics of solar wind turbulence in two-dimensional hybrid simulations
http://aip.metastore.ingenta.com/content/aip/journal/pop/19/2/10.1063/1.3682960
10.1063/1.3682960
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