Geoscience Reference
In-Depth Information
Fig. 9.
As Fig. 5, for MgXI.
while FeXVII and MgXI display a rather uniform distribution over the
planet's disk, consistent with an origin from scattered solar X-rays.
4.
XMM-Newton
EPIC and RGS Spectra
EPIC CCD spectra of Jupiter's auroral zones and of the low-latitude disk
emission were extracted using the spatial selection regions shown in Fig. 10;
their spectral 'mixing' (due to the
XMM-Newton
Point Spread Function)
was corrected for by subtracting appropriate fractions of disk and auroral
spectra, respectively.
12
A combination of two collisional plasma models (
in XSPEC) fits
the EPIC soft X-ray spectra of Jupiter's aurorae well (see Fig. 11 for the
North aurora); the plasma temperatures are
kT
=0
.
17
mekal
±
0.10 keV: the cooler component is required to explain the prominent OVII
emission, and the higher temperature one to describe the higher energy
part of the spectrum. In practise, we use a thin plasma code to mimic the
recombination process inherent to the charge exchange mechanism. A single
mekal
±
0
.
01 and 0.45
0
.
03 keV, with a normalization six times
larger than that required for the auroral spectral component with the same
plasma model (
kT
=0
.
46
±
