Abstract
Spectra of SII emission obtained from early 1976 to mid-1979 in the vicinity of Jupiter show bright emission near the plane of the magnetic equator in the neighborhood of Io's orbit. The emission drops off sharply beyond 6.66 R u from Jupiter, just outside Io's orbit at 5.87 R u . The SII emission is asymmetric in magnetic longitude, being brightest at λ III(1965) = 260°. It is about five times fainter 180° from this position. The longitude of brightest emission is close to the “active sector” where enhanced ionizing currents are expected to exist along Io's flux tube. Rather large variations in the electron density over the SII cloud are reported but the average value is close to previous determinations. The brightest region observed near the ansa of the emission torus had 3.92 < log T e < 4.80, log n e = 4.2 [cm −3] amd column abundance of SII = 1.5 × 10 13 cm −2. The biggest long-term change appears to be in the cloud's sulfur content rather than in its electron temperature or electron density.
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