## 3 Results and Discussion
### Wind Analysis  
The influence of the wind is considered in our study, as shown in [PERSON] et al. (1977) [PERSON] et al. (1977) and [PERSON] et al. (2013) [PERSON] et al. (2013). When the wind flow velocity is below or close to 0.5 m/s and it  
\begin{table}
\begin{tabular}{c c c} \hline \hline
**Ink Flow [mL/s]** & **Plume Height (289 K) [\%] 1** & **Plume Height (301 K) [\%] 1** \\ \hline
0.3 & 81 & 86 \\
0.7 & 106 & 116 \\
1.4 & 129 & 123 \\ \hline \hline \end{tabular}
\end{table}
Table 4: Thermal plume height for non-active (289 K) and active (301 K) resistor.  
Figure 4: Comparison of laminar length fluxes (marked in a green line) for active and non-active resistor: (**a**) non-active resistor (289 K); (**b**) active resistor (301 K).  
\begin{table}
\begin{tabular}{c c} \hline \hline
**Ink Flow [mL/s]** & **Reynold Number** \\ \hline
0.3 & 1239 \\
0.7 & 2817 \\
1.4 & 5408 \\ \hline \hline \end{tabular}
\end{table}
Table 5: Experimental Reynolds number as a function of the ink flow rate.  
directly crosses the RTG (Radioisotope Thermoelectric Generator), a thermal perturbation of between 2 and 5 K can occur. It is important to emphasize that the influence will always be greater for wind flows that hit the RTG directly, heading towards the mast. Given a separation of approximately 2 m between the MMRTG and the mast, and an MMRTG width of approximately 1 m, there will be a potential influence from surrounding elements over an angle of 30\({}^{\circ}\). Considering that the MMRTG has a width of approximately 0.7 m and the distance between it and the mast is around 2 m, the total influence will be 9.9\({}^{\circ}\) rather than 30\({}^{\circ}\). Therefore, the probability that the wind direction vector directly passes through the MMRTG is calculated as \(\frac{30}{360}=\frac{1}{12}\approx 8.33\%\).  
Although, as seen in the mission's database, typical wind speeds on the Martian surface range between 1 and 3 m/s, the objective of this study was to preliminarily verify previous studies on the potential influence of the MMRTG on the measurement instruments mounted on the mast ([PERSON] et al., 2013, 2020 [2,3]). Therefore, the wind speeds selected for this study were below 1 m/s, while respecting the constraints and hypotheses based on the Reynolds number. It is important to emphasize that, as mentioned earlier, these lower wind speeds will show a clear thermal perturbation in the surrounding temperatures.  
Studies conducted by the Department of Aircraft and Space Vehicles at the Technical University of Madrid (School of Aeronautics and Space Engineering) and the National Institute for Aerospace Technology (INTA) ([PERSON] et al., 2022 [7]) indicate that wind flow incidents on the MEDA station generate two types of flow regions around the mast and booms. These two regions are separated by the upstream and downstream sides of the mast. Around the booms, the mast induces a strong influence, creating a large region of disturbed flow, generally characterized by detached flow. This factor can significantly increase the influence of thermal convection on the station and alter measurements if this influencing factor is not considered. The increase in convective influence arises from the enhanced turbulence generated by the wind flow interacting with the mast and booms. This turbulence facilitates greater mixing of air layers, leading to a more effective heat transfer between the atmosphere and the measurement instruments. Additionally, the separation of the flow can create localized areas where warm air accumulates, further affecting the thermal dynamics around the station.