부산대학교 도서관

The Artemis exploration zone lies within 6° latitude of the lunar south pole. It is a topographically complex highland region with a crater >3 times deeper than Earth's Grand Canyon and massifs comparable to Mt. Everest in elevation. To support future landing in this zone, we consider two questions: (i) what elevation changes and surface slopes might be encountered at potential landing sites; and (ii) what type of workload would be required of a ‘walking’ extravehicular activity (EVA) within 2,000 m of a lander? To address the first question, we examined potential Artemis landing sites 001, 004, 007, 011, 102, and 105. At site 001, slopes are generally $< \mathbf{10}^{\mathrm{o}}$ along a ridge towards Shackleton crater, although intervals have slopes approaching 20° and the ridge is bounded by flanks with $> \mathbf{20}^{\mathrm{o}}$ slopes. In the opposite direction, the slope exceeds 10° within 1,000 m of the site. From a landing location near site 001, a ~60 m diameter permanently shadowed region (PSR) suitable for studies of volatile elements is accessible along a 650 m traverse with only a ~20 m section on $\mathbf{a}\sim \mathbf{16}^{\circ}$ slope. If accessed from the west, the same PSR can be entered on $\boldsymbol{\mathrm{a}\sim 8^{\mathrm{o}}}$ slope on a ~850 m traverse. At site 004, traverses would be limited to the rim crest of Shackleton crater, which is bounded by a crater wall with slope ~30° on one side and crater ejecta with slope $\boldsymbol{\geq 15^{\mathrm{o}}}$ on the other side. If one stays on the crater rim, slopes are generally $\boldsymbol{ < 10^{\mathrm{o}}}$. Within 2,000 m of site 001 the relief is ~500 m, while a maximum elevation change along a potential traverse is ~140 m. The corresponding values (relief and maximum traverse elevation change) for other potential landing sites are 1,330 m, 80 m (site 004); 380 m, 90 m (007); 520 m, 90 m (011); 520 m, 40 m (102); and 240 m, 40 m (105). Thus, while the topography of the south polar region is dramatic in places, it offers both productive EVA locations with elevation and slope values not much larger than those experienced by the Apollo crews and locations with progressively more severe topography for the development of EVA exploration capabilities.