Abstract
Abstract. A dispersion relation for parallel propagating whistler mode waves has been applied to the magnetosphere of Saturn and comparisons have been made with the observations made by Voyager and Cassini. The effect of hot (suprathermal) electron-density, temperature, temperature anisotropy, and the spectral index parameter, κ, on the temporal growth rate of the whistler mode emission is studied. A good agreement is found with observations. Electron pitch angle and energy diffusion coefficients have been obtained using the calculated temporal growth rates.
Highlights
The observations of the plasma wave spectrum observed at Saturn by Voyager 1 were first reported by Gurnett et al (1981)
In this study we investigate the whistler mode driven unstable by the electron temperature anisotropy in the presence of a suprathermal power law tail on the electron population (Mace, 1998)
Whistler mode emission observed by Voyager 1 near the ring plane crossing can be accounted for by our calculations
Summary
The observations of the plasma wave spectrum observed at Saturn by Voyager 1 were first reported by Gurnett et al (1981). Whistler mode hiss and chorus emissions were found as Voyager approached the equator at a radial distance of about 5 RS (RS is radius of Saturn). Whistler mode emissions within Saturn’s magnetosphere were detected by the plasma wave instruments on Voyager 2 (Scarf et al, 1982). The ionosphere/magnetosphere produces various plasma instabilities which lead to the emission of waves propagating in the whistler mode waves branch. In the present work we have investigated the whistler mode instability driven by temperature anisotropy in the hot electron component in the magnetosphere of Saturn and compare our results with the whistler mode wave observations by Voyager and Cassini. The plasma parameters in Saturn’s magnetosphere and those used in the present study are discussed in Sect.
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