Science & tech · 1994
What makes Jupiter's auroras emit X-rays?
ROSAT observations support as the most likely cause of Jupiter's X-ray emissions. A model of line emission from sulfur and oxygen ions fit the observed spectrum much better statistically than an model.
Details
This observational study used the Röntgen satellite (ROSAT) high-resolution imager (HRI) and position sensitive proportional counter (PSPC) to observe Jupiter in April 1991 and May 1992. The observations revealed emissions apparently associated with Jupiter's aurora, similar to emissions previously observed by the Einstein Observatory.
The HRI images showed emission mainly from Jupiter's northern hemisphere at all Jovian longitudes observed. There was also some indication that the emission varied with longitude in phase with the well-known ultraviolet modulation of the northern aurora.
The PSPC data revealed a very soft spectrum. The researchers compared the observed spectrum with models of electron bremsstrahlung radiation and line emission from sulfur (S) and oxygen (O) ions. The line-emission spectrum provided a much better statistical fit to the observed spectrum.
These X-ray observations therefore support the hypothesis that ion precipitation is the most likely cause of Jupiter's X-ray emissions. This explanation was first suggested by the Einstein results [Metzger et al., 1983].
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