banner image
No data available.
Please log in to see this content.
You have no subscription access to this content.
No metrics data to plot.
The attempt to load metrics for this article has failed.
The attempt to plot a graph for these metrics has failed.
Nonlinear saturation of relativistic Weibel instability driven by thermal anisotropy
Rent this article for
View: Figures


Image of FIG. 1.
FIG. 1.

(a) Evolution of energy. The solid line represents the magnetic field energy and the dots stand for the kinetic energy of the electrons. (b) Change in perpendicular and parallel temperatures. The solid and dotted lines correspond to parallel and perpendicular temperatures, respectively.

Image of FIG. 2.
FIG. 2.

Electron distribution in momentum space at different times.

Image of FIG. 3.
FIG. 3.

(a) Time evolution of the mode characterized by , which is the most unstable mode in the linear regime. (b) Comparison of the linear growth rate between the simulation result and numerical calculation.

Image of FIG. 4.
FIG. 4.

Electron distribution in the space at different times.

Image of FIG. 5.
FIG. 5.

(a) Magnetic field variation in time. (b) Power spectrum associated with .

Image of FIG. 6.
FIG. 6.

Long-time evolution of magnetic field energy (dash-dotted line) and electrostatic field energy (solid line) in logarithmic vertical scale. The electron kinetic energy is plotted as a dashed line, which, owing to the logarithmic scale, appears almost constant.

Image of FIG. 7.
FIG. 7.

The same as Fig. 5 except that the time scale is over the entire course of the simulation, namely, .

Image of FIG. 8.
FIG. 8.

Spatial structure associated with field (left-hand panel) and the time evolution of spectrum associated with field (right-hand panel).


Article metrics loading...


Full text loading...

This is a required field
Please enter a valid email address
752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Nonlinear saturation of relativistic Weibel instability driven by thermal anisotropy