In previous work, the 27° N Hadley-Apennine site near the Apollo 15 landing area was proposed as the primary near-side lunar base, leveraging local lava tube geometry for subterranean habitat architecture and long-term surface operations. However, the far side of the Moon offers distinct scientific capabilities that no near-side location can match: absolute electromagnetic isolation from Earth and an exceptionally thin crustal barrier separating the surface from the lunar interior.
Humanity has never directly sampled or accessed the mantle of another planetary body. At Mare Moscoviense (27.28° N, 148.12° E), an ancient impact event severely thinned the far-side crust down to a residual thickness under 5 km, making direct physical access to the lunar Moho boundary technically feasible. Crucially, because Mare Moscoviense aligns with the 27° N latitude band, a far-side outpost here directly shares the 27° inclination orbital relay constellation established for the primary Hadley-Apennine base, eliminating the need for dedicated polar relay networks. Reaching Mare Moscoviense provides an unprecedented dual-use foundation for planetary geophysics and deep-space astrophysics.
Unlocking the Lunar Mantle: Scientific Implications
Reaching the exposed mantle interface below Mare Moscoviense alters our understanding of planetary differentiation, thermal evolution, and terrestrial planet formation.
Primary Differentiation and Magma Ocean Models
Current knowledge of planetary interiors relies almost entirely on orbital gravity maps and seismic models. Physical access to pristine, unweathered mantle rock—dominated by Mg-rich olivine and orthopyroxene—delivers a direct ground-truth calibration for the Lunar Magma Ocean (LMO) hypothesis. Analyzing un-degraded crystalline structures reveals exact crystallization sequences and chemical stratification during the Moon's initial cooling phase ∼ 4.5 billion years ago.
Isotopic Fingerprinting and Co-Formation Physics
Samples retrieved from below the surface impact-melt sheet remain pristine, un-contaminated by cosmic ray spallation or surface regolith mixing. Precise laboratory measurements of isotopic ratios (O¹⁷ / O¹⁸, Nd¹⁴² / Nd¹⁴⁴, and W¹⁸²) extracted from pristine mantle cores will provide definitive tests for the Giant Impact Hypothesis, locking down the exact chemical budget and timing of Earth-Moon system co-formation.
Deep Volatile Reservoirs
Subsurface mantle access resolves whether the lunar interior retained magmatic volatiles during its formation. Testing sealed interior samples for trapped hydroxyls (OH⁻), fluorine, sulfur, and noble gas isotopes will determine the primordial volatile budget of the inner solar system, informing models of how early Earth acquired its water and atmospheric precursors.
Post-Excavation Evolution: The Far-Side Observatory Complex
Once the primary mantle penetration and core sampling objectives are secured, the logistical surface infrastructure and communications links at Mare Moscoviense transition into an ultra-quiet astrophysical research hub.
Low-Frequency Radio Astronomy
Located at 148.12° E, Mare Moscoviense sits behind thousands of kilometers of solid lunar mass. This total radio-frequency interference (RFI) shadow blocks Earth's TV, radar, and satellite noise, as well as ionospheric distortion. The site is ideal for deploying distributed dipole antenna arrays operating below 30 MHz—a spectrum band inaccessible from Earth—allowing astronomers to detect the 21 cm neutral hydrogen line and map the universe during the Cosmic Dark Ages prior to star formation.
High-Altitude Optical and Infrared Interferometry
The outer multi-ring mountain walls surrounding Mare Moscoviense rise 2,000-3,000 meters above the central basaltic plain. Positioning cryo-cooled optical and infrared interferometers on these high-albedo peaks provides wide horizon baselines, minimal local thermal re-radiation, and total freedom from atmospheric twinkling. These instruments will enable direct imaging of Earth-sized exoplanets in nearby star systems.
Ultra-Quiet Deep Seismic Node
Coupling broadband seismometers directly to the solid rock face at the base of the subsurface mantle access shaft creates the quietest seismic station in the inner solar system. Free from surface diurnal thermal noise and atmospheric coupling, this node will continuously record deep moonquakes, meteoroid impact stress waves, and free oscillations of the lunar core.
Conclusion
Mare Moscoviense represents the logical second phase of lunar surface development. By combining the orbital geometry of the primary 27° N Hadley-Apennine base with the extreme geology of the far side, this site unifies two major frontiers: unlocking the deep interior history of terrestrial planets and providing an undisturbed, RF-silent platform to observe the early universe.
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