Space Launch System acoustics: Far-field noise measurements of the Artemis-I launch

Gee, Kent L.; Hart, Grant W.; Cunningham, Carson F.; Anderson, Mark C.; Bassett, Michael S.; Mathews, Logan T.; Durrant, J T.; Moats, Levi T.; Coyle, Whitney L.; Kellison, Makayle S.; Kuffskie, Margaret J.

doi:10.1121/10.0016878

Cited by 5 publications

(1 citation statement)

References 9 publications

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“…Although >50 years have passed since the last human presence on the Moon, the 2020s should bring a breakthrough thanks to the Artemis program. Artemis 1 mission, a 25-day flight around the Moon, was completed on December 11, 2022 (Gee et al, 2023). Artemis 2 will perform a similar operation 2024 with a crew (David et al, 2023).…”

Section: Rocks Of the Apollo Programmentioning

confidence: 99%

Lunar ore geology and feasibility of ore mineral detection using a far-IR spectrometer

Ciążela¹,

Bakala²,

Kowaliński³

et al. 2023

Front. Earth Sci.

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Lunar sulfides and oxides are a significant source of noble and base metals and will be vital for future human colonies’ self-sustainability. Sulfide detection (pyrite and troilite) applies to many technological fields and use cases, for example, as a raw material source (available in situ on the Lunar surface) for new solar panel production methods. Ilmenite is the primary iron and titanium ore on the Moon and can provide helium-3 for nuclear fusion and oxygen for rocket fuel. The most important ore minerals have prominent absorption peaks in a narrow far-infrared (FIR) wavelength range of 20–40 μm, much stronger than the spectral features of other common minerals, including significant silicates, sulfates, and carbonates. Our simulations based on the linear mixing of pyrite with the silicates mentioned above indicated that areas containing at least 10%–20% pyrite could be detected from the orbit in the FIR range. MIRORES, Multiplanetary far-IR ORE Spectrometer, proposed here, would operate with a resolution down to <5 m, enabling the detection of areas covered by 2–3 m2 of pyrite (or ilmenite) on a surface of ∼17 m2 from an altitude of 50 km, creating possibilities for detecting large and local smaller orebodies along with their stockworks. The use of the Cassegrain optical system achieves this capability. MIRORES will measure radiation in eight narrow bands (0.3 µm in width) that can include up to five bands centered on the ore mineral absorption bands, for example, 24.3, 24.9, 27.6, 34.2, and 38.8 µm for pyrite, marcasite, chalcopyrite, ilmenite, and troilite, respectively. The instrument size is 32 x 32 x 42 cm, and the mass is <10 kg, which fits the standard microsatellite requirements.

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Section: Rocks Of the Apollo Programmentioning

confidence: 99%