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.
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