  Soft x-ray emissions induced by solar wind ions that collide with neutral
material in the solar system have been detected around planets, and were
proposed as a remote probe for the solar wind interaction with the Martian
exosphere. A multi-fluid three-dimensional magneto-hydrodynamic model is
adopted to derive the global distributions of solar wind particles. Spherically
symmetric exospheric H, H$_2$, He, O, and CO$_2$ density profiles and a
sophisticated hybrid model that includes charge-exchange and proton/neutral
excitation processes are used to study the low triplet line ratio
$G=\frac{i+f}{r}$ (0.77$\pm$0.58) of O VII and total x-ray luminosity around
Mars. We further calculate the emission factor $\alpha$-value with different
neutrals over a wide ion abundance and velocity ranges. Our results are in good
agreement with those of previous reports. The evolution of the charge stage of
solar wind ions shows that sequential recombination due to charge-exchange can
be negligible at the interaction region. This only appears below the altitude
of 400~km. The anonymous low disk $G$ ratio can be easily explained by the
collisional quenching effect at neutral densities higher than
10$^{11}$cm$^{-3}$. However, the quenching contribution is small in Mars'
exosphere and only appears below 400~km. Charge-exchange with H$_2$ and N$_2$
is still the most likely reason for this low $G$-ratio. X-ray emissivity maps
in collisions with different neutrals differ from each other. A clear bow shock
in the collision with all the neutrals is in accordance with previous reports.
The resulting total x-ray luminosity of 6.55~MW shows a better agreement with
the XMM-Newton observation of 12.8$\pm$1.4~MW than that of previous
predictions.
