Since a spatially one-dimensional simulation system along a magnetic field line has been used in these simulations, whistler-mode waves of purely parallel propagation are treated.
The arrows on the graph indicate the solution of the non-linear three-wave interaction, L + w → T, for whistler-mode waves of 0.25ωce.
This shows that the three-wave coupling of L + w → T can take place with whistler-mode waves of the frequency of ωw = 0.25 Fig. 6.
In run 1, the simulation result reveals that whistler-mode waves of the different wave frequencies propagate in the different ray path in the region away from the magnetic equator.
In run 1, the simulation result revealed that whistler-mode waves of different wave frequencies propagated in the different ray path in the region away from the magnetic equator.
In this study, the frequency of whistler-mode waves of 0.25 ωce at which the group velocity is maximal is taken account, whereas the frequency of whistler-mode waves was assumed approximately 0.1 ωce in previous studies of fiber bursts (e.g., Chernov et al., 2008).
In present paper whistler mode waves in magnetosphere of Saturn have been investigated.
The method using the hybrid code does not assume the existence of normal mode waves in the kinetic regime a priori.
Then, in the exponential step mode, square waves of 32, 64, 128, 256, and 512 Hz are sequentially outputted and responses are acquired.
In the case of the linear step mode, rectangular waves of 32, 64, 96, 128, and 160 Hz are sequentially outputted with the same initial frequency and step number and responses are acquired.
