Nozette S, Lichtenberg C L, Spudis P, Bonner R, Ort W, Malaret E, Robinson M, Shoemaker E M. Microwave imaging of Mercury’s thermal emission at wavelengths from 0.3 to 20.5 cm. A new, lower value of total solar irradiance: Evidence and climate significance. The Oxford 3D thermophysical model with application to PROSPECT/Luna 27 study landing sites. King O, Warren T, Bowles N, Sefton-Nash E, Fisackerly R, Trautner R. Interpretation of the lunar microwave brightness temperature spectrum: Feasibility of orbital heat flow mapping. Ancillary data services of NASA’s navigation and ancillary information facility. Global regolith thermophysical properties of the Moon from the diviner lunar radiometer experiment. Hayne P O, Bandfield J L, Siegler M A, Vasavada A R, Ghent R R, Williams J P, Greenhagen B T, Aharonson O, Elder C M, Lucey P G, Paige D A. Lack of exposed ice inside lunar south pole Shackleton crater. Haruyama J, Ohtake M, Matsunaga T, Morota T, Honda C, Yokota Y, Pieters C M, Hara S, Hioki K, Saiki K, Miyamoto H, Iwasaki A, Abe M, Ogawa Y, Takeda H, Shirao M, Yamaji A, Josset J L. Illumination and communication conditions at the Mons Rümker region based on the improved Lunar Orbiter Laser Altimeter data. Hao W F, Zhu C, Li F, Yan J G, Ye M, Barriot J P. Temperatures near the lunar poles and their correlation with hydrogen predicted by LEND. Gläser P, Sanin A, Williams J P, Mitrofanov I, Oberst J. Illumination conditions at the lunar poles: Implications for future exploration. Gläser P, Oberst J, Neumann G A, Mazarico E, Speyerer E J, Robinson M S. Numerical simulation of effective solar irradiance and temperatures at simple crater of lunar dayside. Analyzing the ages of south polar craters on the Moon: Implications for the sources and evolution of surface water ice. 483ĭeutsch A N, Head III J W, Neumann G A. Physical Properties of the Lunar Surface. Nature, 443: 835–837Ĭarrier III W D, Olhoeft G R, Mendell W. No evidence for thick deposits of ice at the lunar south pole. Icarus, 208: 558–564Ĭampbell D B, Campbell B A, Carter L M, Margot J L, Stacy N J S. Illumination conditions of the south pole of the Moon derived using Kaguya topography. Sol Energy, 31: 439–444īussey D B J, McGovern J A, Spudis P D, Neish C D, Noda H, Ishihara Y, Sørensen S A. Solar geometry for fixed and tracking surfaces. Lunar surface roughness derived from LRO Diviner radiometer observations. We suggested four trade-off sampling sites with suitable temperatures and gradual slopes.īandfield J L, Hayne P O, Williams J P, Greenhagen B T, Paige D A. To further ensure normal rover movement, we provided a map of suitable temperature sites and found that these locations exist not only in the Shackleton crater’s inner wall, but also outside the crater. There are suitable temperature locations which have a warm surface but cold subsurface to preserve water ice. The permanently shadowed regions can be as cold as 25 K, and such extreme coldness is a hazard to the rover. The locations receiving more solar radiation show a temperature larger than the threshold (∼112 K) of ice stability. This difference indirectly implies that the conductivity of the lunar regolith is inefficient. Our results also indicate that the surface temperature is more sensitive to transient illumination, but the subsurface temperature is more likely to be associated with the accumulated illumination. Our results indicate the temperature in the permanent shadow region remains nearly constant, thus validating the stability of our estimated initial temperature. Using the real-time illumination and the distributed 1-D thermal diffusion model, we continuously evaluated the regolith temperature for more than 20 years to stabilize the temperature, and selected the temperature of the end time as the initial value used in a thermal study set for Jand May 8, 2027. The map indicates the illuminated inner wall of the Shackleton crater is close to 27% of the whole, meaning that the rover will likely receive solar radiation during its movement. In addition, we estimated an accumulated illumination map for the period of likely rover movement. We used the NASA’s SPICE system to evaluate the terrain obscuration effect on real-time illumination the resulting illumination map resembles previous studies, validating the methodologies used in our study. This study focuses on the illumination and temperature at China’s next lunar candidate landing site Shackleton crater.
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