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