The Dynamic Atmosphere Energy Transport (DAET) climate model, a
mathematical model previously applied to a study of Earth’s climate, has
been adapted to study the climatic features in the low-pressure,
dust-prone atmosphere of the planet Mars. Using satellite data observed
for Martian Year 29 (MY29), temperature profiles are presented here that
confirm the studies of prior authors of the existence on Mars of a
tropical solar-energy driven zone of daytime atmospheric warming, that
both diurnally lifts the tropopause and follows the annual latitudinal
cycle of the solar zenith. This tropical limb of ascending convection is
dynamically linked to polar zones of descending air, the seasonal focus
of which is concentrated over each respective hemisphere’s polar winter
cap of continuous darkness. An analysis of the MY29 temperature data was
performed to generate an annual average surface temperature metric that
was then used to both inform the design of and to constrain the
computation of the DAET climate model. The modelling analysis suggests
that the Martian atmosphere is fully transparent to surface emitted
thermal radiant energy. The role of lit hemisphere surface reflectance
provides an energy boost to the dust-prone surface boundary layer at
grazing-angle latitudes. This backlighting process of quenched solar
energy capture ensures that the Martian climate operates as a black-body
system. The high emissivity solar illuminated hemispheric surface heats
the atmosphere by direct thermal conduction followed by a process of
adiabatic convection across the planetary surface. It is the non-lossy
process of adiabatic convection that results in the development and
maintenance of a flux-enhanced atmospheric energy reservoir which
accounts for the 2 Kelvin Atmospheric Thermal Effect in the Martian
troposphere.