## 2 Materials and Methods
### Physics-Based Challenges  
As it was already mentioned, there are several physics-based challenges restricting the outpost development on the Moon and Mars. These challenges comprise microgravity, cryogenic temperature, the non-existence of adequate atmospheric pressure, a lack of magnetic fields, extreme surface radiations, and micrometeoroid impacts. Figure 3 shows these challenges. Any conceptual lunar or Martian outpost must meet the specifications related to these challenges. In the case of access to inclusive data related to these challenges, artificial intelligence approaches can be used to analyze the effect of these challenges on extraterrestrial outpost construction [27]. The Earth's diameter is relatively two times Mars's diameter and four times the Moon's diameter [28]. Moreover, gravitational acceleration on the lunar and Martian surface is, respectively, equal to 1.62 m/s\({}^{2}\) and 3.71 m/s\({}^{2}\); these values are significantly less than 9.81 m/s\({}^{2}\) on the Earth [28]. This phenomenon is known as microgravity imposing many limitations on habitation development. Because of microgravity, a human habitat may undergo instability problems [29]. Consequently, to address this challenge, there is a need for a foundation that fastens the habitat to the regolith beneath; however, the lunar and  
Figure 3: Primary physics-based challenges in the construction of lunar and Martian outposts. Martian regolith is very cohesionless (order of a few kPa) [9]; therefore, to reach a depth with stiff regolith, drilling tools capable of penetrating into the lower depths must be deployed. As a result, there will be a need to apply much greater forces to drill the lunar and Martian regolith [30; 31]. Therefore, the first challenge is the microgravity-derived instability of the habitat, which calls for stronger, weightier, and bulkier drilling machinery. The atmospheric temperature on the Moon's poles amounts to \(-230\)\({}^{\circ}\)C, and on Mars's poles, it reaches \(-140\)\({}^{\circ}\)C [10]. Such cryogenic conditions create a diverse spectrum of challenges in the development of extra-terrestrial outposts [32; 33]. To address this issue, a vital action is the thermal insulation of the interior parts of the outpost from harsh exterior atmospheric conditions. To carry this out, appropriate insulators must be transported and deployed, thereby increasing transportation costs. Furthermore, cryogenic temperatures induce thermal stresses within the materials [34; 35]. Therefore, adequate resistance to cryogenic temperatures is another criterion for the selection of construction materials [20]. This matter precludes countless raw materials from being adopted in lunar and Martian outpost construction. While on Earth, the atmospheric pressure (at room temperature) is around 100 kPa, the tenuous Martian atmosphere has a very low pressure equal to 0.6 kPa [36]. Even worse, the atmospheric pressure on the lunar surface falls between 4 kPa-10 kPa (during days) and 7 kPa-10 kPa (during nights). The lack of atmospheric pressure on Martian and lunar surfaces exacerbates the conditions for outpost development. Most importantly, the shortage of atmospheric pressure curtails the applications of fluids in the construction process [20]. Thus, many terrestrial-based fuels, hydraulic oils, additives, binders, etc., are only applicable under stringent specifications. Furthermore, the non-existence of atmospheric pressure makes the Moon and Mars susceptible to micrometeoroid collisions and solar/cosmic radiation [37]. This obstacle calls for the adoption of a protective layer on the outpost. To meet this issue, a number of researchers have proposed the construction of underground structures, such as the expansion of lava tubes and tunnel construction using tunnel boring machines (TBMs) [38; 39; 40]. On a certain planet, the magnetic field stems from its core conditions, i.e., the core composition, lack or presence of plate tectonics, and water repartition [41].