## 2 Materials and Methods
### Physics-Based Challenges
On Earth, the magnetic field protects human life from solar and galactic radiation [42]. In other words, Earth's magnetic field constitutes a magnetic shield (magnetosphere) that spans several tens of thousands of kilometres from the Earth's surface towards space [42] and prevents charged particles from stripping away the upper atmosphere, i.e., most importantly, the Ozone layer [43]. Nevertheless, Mars, the Moon, and even Venus suffer from their magnetic fields in order to protect their surfaces from solar winds, cosmic rays, and micrometeoroid impacts [20; 28]. On Mars, the photos captured by the Curiosity rover have confirmed the early presence of water streams, forming a delta area in the craters. From this observation, the former existence of the Martian magnetic field was deduced [44]. [PERSON] et al. have ascribed the water loss and obliteration of the Martian atmosphere (life) to such dramatic reductions in the Martian core's magnetic field [44]. Surface radiation in lunar and Martian environments is far more extreme than Earth's [45]. Solar winds, solar flares, and cosmic rays are three major spectra of radiation that reach the Moon and Mars's surfaces [46]. Of all these radiation types, solar winds are further hazardous for the outpost's inhabitants. From the site-selection standpoint, the location of the outpost must be chosen in regard to the minimum degree of such solar winds. On the Moon's surface, a typical lunar day relatively lasts 28 Earth days [47]. In the lunar polar regions in which the water-bearing regolith has already been reported [8; 20], the solar wind reaches the surface with a roughly horizontal angle [20]. Hence, the construction of an outpost in such locations effectively curtails the solar wind. In addition, for further a reduction in incoming solar wind, the outpost can be covered by a protective regolith layer [20]. The thickness of the regolith layer can range from 1.5 m to 2 m [20]. Furthermore, some membranes, such as lightweight polyimides, which are very suitable for extraterrestrial inflatable structures, can hinder solar radiation [48]. Polyimide also hasgood transparency, and it can be utilized as outpost windows, permitting sunlight to shine into the outpost [48]. Seismic events on lunar and Martian surfaces mainly originated from two sources: meteoroid impacts and lunar/Martian ground motions (quacks) [49]. In this paragraph, we only describe the effects of meteoroid impacts on lunar/Martian outpost development because the topic of ground motions on the Moon and Mars is too broad to be elaborated in detail here. Due to the non-existence of magnetic and atmospheric barriers, potential meteoroids strike lunar and Martian surfaces at high speeds. A wealth of information pertinent to the weight, size, speed, and location of the lunar meteoroids was obtained during the years of 1970-1977 via a series of seismometers employed on the Moon's surface [50]. According to those data, the most frequent meteoroids reaching the lunar surface have a mass of less than 0.5 kg [50]. On the other hand, collisions of meteoroids heavier than 1 ton are very scarce [51]. The average velocity of the striking meteoroids amounts to 22.5 km/s (to compare to this speed, a bullet is released from a rifle at a speed that is approximately equal to 2 km/s) [52]. During each year, more than 4000 impactors with an average weight of 1 kg may hit the Moon's surface. Furthermore, from the site-selection viewpoint, it can be said that the collision locations of bigger impactors are not regularly distributed on the Moon's surface although they demonstrate clustering [53]. Hence, it is of paramount significance to consider the possibility of meteoroids collisions with the outpost's structure. Before the 2000s, researchers chiefly proposed Kevlar composites in their conceptual structures because of their protection against meteoroid impacts and their lightness and high tensile strength. [PERSON] et al.