Observations of the Jovian X-ray Emission by Chandra and XMM Newton

Details Observations of the Jovian X-ray Emission by Chandra and XMM Newton Observations of the Jovian X-ray Emission by Chandra and XMM Newton

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm41b1667c&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM41B-1667

Physics

5706 Aurorae, 5737 Magnetospheres (2756), 6220 Jupiter

Scientific paper

Three different kinds of aurorae are generally seen in UV and near-IR observations of Jupiter: (1) Aurorae at the satellite footprints (2) the main oval and (3) transient signatures at higher latitudes called polar emissions. Jovian x-rays are primarily associated with the polar emissions, and are particularly intense in a "hot spot" region near 60-70 degrees north latitude and 160-180 degrees system III longitude. The auroral x- rays are primarily due to line emission from precipitating energetic O and S ions (300-800 eV photons), with a small fraction due to electron bremsstrahlung (> 2000 eV photons). Here we present new x-ray observations obtained simultaneously by Chandra and XMM Newton at the end of February 2007, during the New Horizons Jupiter flyby. These observations confirm the presence of O and S emissions in separate bands around 500-700 eV and 200-400 eV respectively, with only minor spatial and temporal variations in the brightness ratio between the two bands. These observations thus indicate a rather steady O/S ratio in the magnetospheric source region of the x-ray aurora (thought to be near the dayside magnetopause).

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