Investigation of Io's Auroral Hiss Emissions Due To Its Motion in Jupiter's Magnetosphere

Details Investigation of Io's Auroral Hiss Emissions Due To Its Motion in Jupiter's Magnetosphere Investigation of Io's Auroral Hiss Emissions Due To Its Motion in Jupiter's Magnetosphere

2011-09-15

arxiv.org/abs/1109.3264v2

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

Scientific paper

The left-hand side of the auroral hiss emission observed by Galileo has a frequency time shaped very similar to the funnel shape observed in the earth's auroral region. This close similarity indicates that we can use the whistler-mode propagation near resonance cone to locate the emission source. In this paper the general characteristic of the whistler mode are discussed. Then the position of the emission source has been investigated using a geometry method that takes into account the Galileo's trajectory. Initially it is assumed the source is a point. Then the possibility of sheet source aligned along the magnetic field lines which are tangent to the surface of Io is investigated. Both of two types of sources show that the whistler mode radiation originates very close to the surface of the Io.

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