  A diagnosis of the Ar densities measured by the Neutral Gas and Ion Mass
Spectrometer aboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) and the
temperatures derived from these densities shows that solar activity, solar
insolation, and the lower atmospheric dust are the dominant forcings of the
Martian thermosphere. A methodology, based on multiple linear regression
analysis, is developed to quantify the contributions of the dominant forcings
to the densities and temperatures. The results of the present study show that a
100 sfu (solar flux units) change in the solar activity results in approx. 136
K corresponding change in the thermospheric temperatures. The solar insolation
constrains the seasonal, latitudinal, and diurnal variations to be
interdependent. Diurnal variation dominates the solar insolation variability,
followed by the latitudinal and seasonal variations. Both the global and
regional dust storms lead to considerable enhancements in the densities and
temperatures of the Martian thermosphere. Using past data of the solar fluxes
and the dust optical depths, the state of the Martian thermosphere is
extrapolated back to Martian year (MY) 24. While the global dust storms of MY
25, MY 28 and MY 34 raise the thermospheric temperatures by approx. 22-38 K,
the regional dust storm of MY 34 leads to approx. 15 K warming. Dust driven
thermospheric temperatures alone can enhance the hydrogen escape fluxes by
1.67-2.14 times compared to those without the dust. Dusts effects are
relatively significant for global dust storms that occur in solar minimum
compared to those that occur in solar maximum.
