Opracowanie koncepcji uzyskiwania strumieni gazu o podwyższonej zawartości helu na membranach

Janocha, Andrzej; Badawczy, Instytut Nafty i Gazu – Państwowy Instytut

doi:10.18668/ng.2020.10.07

Cited by 1 publication

(1 citation statement)

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“…A process that allows both oxygen and metals to be produced from ilmenite has been reported by Schwandt et al (2012). Further works focus on separating various gases obtained from ilmenite or regolith (Schlüter et al, 2021), helium from other gases (Janocha, 2020), and 3 He from 4 He (Kempiński et al, 2019). Therefore, ilmenite is currently being studied as a resource (Johnson et al, 1999;Fa and Jin, 2007;Kim et al, 2019).…”

Section: Potential Resources Of the Moonmentioning

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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