![]() |
Figure 1:
Solar maximum and solar minimum full sky monochromatic for the O7+ line at 0.65 keV and the O5+ line at 0.08 keV.
The observer is situated
at 75![]() ![]() ![]() ![]() ![]() |
Open with DEXTER |
![]() |
Figure 2: Ratio between the total ion density (including secondary CX sources) and primary ion density as a function of distance from the Sun. |
Open with DEXTER |
![]() |
Figure 3: Solar wind streamlines calculated with the Izmodenov & Alexashov (2003) model. Arrows mark the three LOS for which the contribution of the outer heliosphere has been calculated and presented in Fig. 4. |
Open with DEXTER |
![]() |
Figure 4: Contribution of the heliosheath upwind (red) and crosswind (black), and the heliotail (blue) to a heavy SW ion emission. Intensity, in units of 10-9 erg cm-2 s-1 sr-1, is presented as a function of distance r to the Sun (in AU). See location of (a) to (f) points in Fig. 3. |
Open with DEXTER |
![]() |
Figure 5: Heliospheric EUV a) and X-ray b) emission spectra for an observer located upwind pointing in three different lines of sight: north ecliptic pole in blue, south ecliptic pole in red and equatorial antisolar LOS in green. Plain lines correspond to solar minimum conditions and dashed lines correspond to solar maximum conditions. Units are photons cm-2 s-1 sr-1 eV-1. |
Open with DEXTER |
![]() |
Figure 6: Same as Fig. 5 but for an observer located downwind. Units are photons cm-2 s-1 sr-1 eV-1. |
Open with DEXTER |
![]() |
Figure 7: Solar Wind enhancement localization for the start of the XMM HDFN X-ray observation. |
Open with DEXTER |
![]() |
Figure 8: Various parameters' temporal profiles, before, during and after the June 1, 2001 HDFN observation. Periods where no X-ray observations of HDFN are available are crosshatched in the graphs. Lower panels show SW input parameters: The dashed black line shows the proton flux enhancement, estimated as a step function, in units of SPFU (see text for further explanation). The dashed red line and the dashed blue line show the O7+/O6+ and the O8+/O7+ ratio evolution respectively. Left panel: O7+/O6+ and O8+/O7+ ratios derived from ACE measurements. Right panel: O8+/O7+ ratio implied by Snowden et al. analysis. Upper panels show X-ray emission temporal profiles for the two cases considered: The plain black line shows the simulation result for X-ray energy flux in the energy range 0.52-0.75 keV. The plain red and blue lines show X-ray energy fluxes for the two major spectral lines in this energy range: the O VII 0.56 keV and O VIII 0.65 keV lines respectively. The green horizontal lines show average high and low heliospheric energy fluxes in the energy range 0.52-0.75 keV by XMM data fit, assuming there is no heliospheric contribution in the low X-ray emission state (SCK04). The purple horizontal lines show equivalent averages assuming that there is no cosmic background contribution, only particle background (this study). Energy fluxes are all presented in units 10-9 ergs cm-2 sr-1 s-1. |
Open with DEXTER |
![]() |
Figure 9: Line of Sight (LOS) Geometry. |
Open with DEXTER |
![]() |
Figure 10:
Iso-emissivity contour maps up to 15 AU for solar
minimum conditions. Left column corresponds to the sum of the ion
O5+ lines at 0.072 and 0.082 keV and right column to the sum of the ion O6+ lines at 0.561, 0.569 and 0.574 keV.
Top panels correspond to the plane (x, y) defined by the vectors
(74![]() ![]() ![]() ![]() ![]() ![]() |
Open with DEXTER |
![]() |
Figure 11:
Solar maximum and solar minimum full sky monochromatic emission maps. The two lines here are the 0.65 keV (O7+) and the 0.08 keV
(O5+). The observer is situated at 121![]() ![]() ![]() ![]() |
Open with DEXTER |
![]() |
Figure 12:
Same as Fig. 11 for an observer
at 165![]() |
Open with DEXTER |
![]() |
Figure 13:
Same as Fig. 11 for an observer
at 211![]() |
Open with DEXTER |