Abstract
The relativistic electron energy in few MeV range, trapped in the Jovian magnetosphere emit electromagnetic waves in wide radio frequency domain which escapes the generation region and propagates towards the Earth’s atmosphere. The flux density of the emission is a function of the electron distribution (spatial and angular), the energy spectrum of the electron, the magnetic field strength and configuration. The measured spectral power density of high energetic electrons and its distribution with frequency can be used to find out the distribution of relativistic electrons in the inner magnetosphere having the range LJ =3 Jovian radius. In present communication the variation of radiated power per electron with energy through the synchrotron radiation process have been shown and discussed. The simulated flux density is compared with corresponding recent emitted radio spectrum data available from Cassinni flyby. The investigation enables us to explain the mechanism and characteristic properties of Jovian magnetosphere.
Highlights
In 1950’s, radio emissions from the Jupiter were recorded in two frequency bands referred as decametric (DAM) and decimetric (DIM)
In order to explain the observed power received on the surface of the Earth and onboard spacecraft emitted from Jovian magnetosphere it is essential to know the density, energy and pitch angle distribution of radiating particles as well as magnetic field variation in the generation region
The maximum flux density of 10-26 W m-2 Hz-1 lies around frequency 1 GHz for energy 100 MeV and 2 GHz for 200 MeV, which is in close consistency with observed radio spectrum
Summary
In 1950’s, radio emissions from the Jupiter were recorded in two frequency bands referred as decametric (DAM) and decimetric (DIM). Levin et al [25] compared the DG model with synchrotron emission observations and showed that DG model did not accurately describe the high-energy (>1 MeV) electron population present in the Jupiter’s inner radiation belt (< 4 RJ).
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