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In-Depth Information
Fig. 13. Top panel:
XMM-Newton
EPIC (upper curve) and RGS (lower curve) soft
X-ray spectra of Jupiter (full planet) and best fit with a combination of
models.
Bottom panel: Individual spectral channel contributions to the
χ
2
value (thin line: EPIC;
thick line: RGS).
mekal
5. Discussion and Conclusions
Our
XMM-Newton
results support the view that Jupiter's auroral emis-
sions originate from precipitating energetic heavy ions, producing soft
X-rays by charge exchange. They presently favor a solar wind scenario
10
while
Chandra
data
7
are suggestive of a magnetospheric origin. A pure
solar wind scenario, though, is probably excluded because it would lead
to Ly
α
production in excess of what is observed.
8
More detailed model-
ing is being carried out to establish the true origin of the X-ray lines, and
studies are underway to resolve the differences.
12
It is conceivable that
both scenarios play a role in what is certainly a very complex planetary
structure.
Acknowledgments
This work is based on observations obtained with
XMM-Newton
,anESA
science mission with instruments and contributions directly funded by ESA
