Evaluating Seismic Ambient Noise Techniques for Imaging Lava Tubes on the Moon

Abstract Detecting and characterizing lava tubes is a key objective of upcoming lunar missions. While evidence for their presence exists, their precise dimensions and depths remain uncertain. This study evaluates the potential of seismic ambient noise methods, such as seismic interferometry, H/V spectral ratios, distributed acoustic sensing (DAS), and rotational measurements, for detecting and imaging lava tubes on the Moon. To achieve this, we perform 2D numerical simulations using a digital model of the shallow subsurface, incorporating lava‐tube–like voids. In addition to simplified geometries for evaluating resolution limits, the Marius Hills skylight is modeled to investigate a realistic scenario. Hereby, phase velocity dispersion curves of Rayleigh waves are extracted from DAS and rotational data, while group velocity dispersion curves are derived from interferometry. All methods show sensitivity to voids, with reliable estimates of roof thickness, but the total depth of the lava tube remains more difficult to constrain. Moreover, resolving structures deeper than 10 m requires ambient noise at frequencies below 1 Hz. Such frequencies lie below the typical range of thermal moonquakes, which are the main source of ambient seismic noise on the Moon. These results suggest that robust imaging of lunar lava tubes will likely require combining multiple ambient noise techniques and complementary geophysical approaches.