Simulating Jupiter's X-ray Emission In The Laboratory

Details Simulating Jupiter's X-ray Emission In The Laboratory Simulating Jupiter's X-ray Emission In The Laboratory

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0317f&link_type=abstract

American Astronomical Society, AAS Meeting #212, #3.17; Bulletin of the American Astronomical Society, Vol. 40, p.187

Astronomy and Astrophysics

Astronomy

Scientific paper

Precipitation of fast, highly charged ions is thought to be a mechanism for the production of copious amounts on X rays observed by the Chandra X-ray Observatory from Jupiter's polar regions. The energy of the observed X rays suggests emission from the K-shell of oxygen ions and the L-shell of sulfur ions. We have used the LLNL SuperEBIT facility to produce open-shell sulfur ions and to study their X-ray emission as they recombine via charge exchange. The X-ray emission was monitored with the ECS microcalorimeter, which was specially modified to record the resulting L-shell low-energy X rays between about 200 and 600 eV. Comparison of these spectra with those obtained under electron-impact excitation show marked differences. In particular, a strong enhancement of the emission from levels with high principal quantum number is found. Such an enhancement is not seen in the Chandra spectra, which supports suggestions that that particular emission does not come from sulfur.
Part of this work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and NASA grants to LLNL, SAO, and GSFC.

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