Simulation der Temperaturverhältnisse am Südpol des Mondes – Abstrakt
The purpose of this work is to show the theoretical thoughts needed to create
a temperature simulation for the moon and to compare a currently applied model
(Vasavada, 2012) in the specific conditions of the southpole of the moon with
measured data and to adapt it for this region if needed.
Vasavada’s model was not created to archive high areal resolution, he assumed
the moon as a perfect sphere, with mountains and craters being ignored. At low
angle of incidence of the sun the real relief of the surface is important for the
local temperatures, so the implementation of the TU München uses a separate
calculation of the radiation including the real relief of the surface.
An extensive comparison with measured data shows that Vasavada’s model differs
from measured data in average 33 Kelvin. To see the effect of change of the
simulation parameters, multiple simulations with different simulation parameters
were performed, some of which showed big differences and some did not.
At first it became noticeable that due to a programming mistake the temperatures
got to high. More improvements brought the increase of the Albedo of the surface
and the change of the temperatures in the beginning of the simulation.
In total, the average difference was reduced by about 13 K.