There could be more ice on the Moon than we thought

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The Vikram lander on the lunar surface with the ChaSTE probe deployed. Credit: ISRO (Indian Space Research Organisation).
The Vikram lander on the lunar surface with the ChaSTE probe deployed. Credit: ISRO (Indian Space Research Organisation).

There could be ice a few centimetres below the Moon’s surface in more areas of the lunar polar regions than previously thought, according to international researchers who say this could be useful for future long-term exploration missions that require the presence of ice to provide water. The team analysed temperature readings taken at the lunar surface in 2023 by the Indian Chandrayaan-3 mission. The authors found that temperatures at the landing site, a Sun-facing slope angled at 6°, peaked at 355 Kelvin (82 degrees Celsius) and dropped to 105 Kelvin during the lunar night. However, a lower peak temperature of 332 Kelvin (59 degrees Celsius) was measured on a flat region approximately one metre from the lander. Using this data, the team developed a model to estimate how slope angle could affect surface temperature, and found for slopes facing away from the Sun and towards the nearest pole, a slope with a greater than 14° angle may be cool enough for ice to accumulate close to the surface.

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From: Springer Nature

Planetary science: More potential locations for ice on Moon *IMAGES*

Ice may be present a few centimetres below the Moon’s surface in more areas of the lunar polar regions than was previously thought due to large, yet highly localised, variations in surface temperatures. The results, published in Communications Earth & Environment, are derived from direct measurements taken at the lunar surface in 2023 by the Indian Chandrayaan-3 mission.

Future long-term exploration (or habitation) of the Moon will likely depend on the availability of ice to provide water, with the likelihood of ice formation in a lunar area directly affected by the surface temperature. The only previous direct measurements of the lunar surface temperature were taken during the Apollo missions of the 1970s. However, these missions landed near the equator, several thousand kilometres from proposed landing sites for future manned missions, and where terrain slope has little effect on temperature.

Durga Prasad and colleagues analysed temperature readings taken at the lunar surface and to a depth of 10 centimetres below by ChaSTE — a temperature probe experiment on Chandrayaan-3’s Vikram lander, which touched down at the edge of the south polar region (approximately 69 ° south). The authors found that temperatures at the landing site, a Sun-facing slope angled at 6 °, peaked at 355 Kelvin (82 degrees Celsius) and dropped to 105 Kelvin during the lunar night. However, a lower peak temperature of 332 Kelvin (59 degrees Celsius) was measured on a flat region approximately 1 metre from the lander.

The authors used the collected data to derive a model of how slope angle affects surface temperature at high lunar latitudes similar to the landing site. The model indicated that, for slopes facing away from the Sun and towards the nearest pole, a slope with a greater than 14 ° angle may be cool enough for ice to accumulate close to the surface. This is similar to conditions at the lunar poles, including those at the proposed landing sites for NASA’s manned Artemis missions near the lunar south pole. The authors therefore suggest that areas on the Moon where ice can form may be more numerous and easier to access than previously thought.

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conference:
Communications Earth & Environment
Research:Paper
Organisation/s: Physical Research Laboratory, India
Funder: ChaSTE experiment is supported by Department of Space, Government of India and jointly developed by Space Physics Laboratory (SPL), Vikram Sarabhai Space Centre (VSSC), Thiruvananthapuram and Physical Research Laboratory (PRL), Ahmedabad. We acknowledge the support provided by various entities of Space Applications Centre (SAC), Ahmedabad during various phases of development, test and evaluation of Front-End electronics of ChaSTE.We are immensely grateful to Dr. Veeramuthuvel andthe entireChandrayaan-3 team, inparticularURRaoSatellite Centre (URSC), Bangalore; ISRO Telemetry, Tracking and Command Network (ISTRAC), Bangalore; Satish Dhawan Space Centre (SDSC), Sriharikota, for their support during various phases of design, development and operations of ChaSTE.We are immensely thankful to M. Srikanth, Rethika andmission operations teamfor their support in flawlessly executing various operational phases of ChaSTE. We specifically thank OHRC team at SAC, NAVCAM teams at LEOS and Data Processing team at ISTRAC for their support. We thank Dr. Santosh Vadawale, Dr. Megha Bhatt, Dr. Shanmugam, Dr. Varun Sheel and other colleagues at PRL for their discussions and suggestions. Weare extremely thankful toDr. S. Somnath,Chairman, ISRO, for his continued support to this experiment right from its inception. We are extremely indebted toShri. A.S. KiranKumar,Chairman,PRLCouncil, for his meticulous review of ChaSTE during its various phases of development and in particular for his timely support and suggestions during mission operations. A.B. was J.C. Fellow during this work. A.G. is a PhD research student supported by Govt. of India’s DST-INSPIRE fellowship grant during the period of this work and we thank DST for the same. The computations were performed ontheParamVikram-1000High PerformanceComputingCluster of the Physical Research Laboratory (PRL). We thank the anonymous reviewers for their comments and suggestions. No permissions are required for geological samples used in the present study.
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