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The unequal distribution of volcanic products between the Earth-facing lunar side and the farside is the result of a complex thermal history. To help unravel the dichotomy, for the first time a lunar landing mission (Chang'e-4, CE-4) has targeted the Moon's farside landing on the floor of Von Kármán crater (VK) inside the South Pole-Aitken (SPA). We present the first deep subsurface stratigraphic structure based on data collected by the ground-penetrating radar (GPR) onboard the Yutu-2 rover during the initial nine months exploration phase. The radargram reveals several strata interfaces beneath the surveying path: buried ejecta is overlaid by at least four layers of distinct lava flows that probably occurred during the Imbrium Epoch, with thicknesses ranging from 12 m up to about 100 m, providing direct evidence of multiple lava-infilling events that occurred within the VK crater. The average loss tangent of mare basalts is estimated at 0.0040-0.0061. The authors here report results from the ground-penetrating radar onboard the Yutu-2 rover from the Chagn'E 4 mission. The study presents up to 330 m deep subsurface structure of the Von Karman Crater inside the South Pole Aitken Basin. [ABSTRACT FROM AUTHOR]

On 3 January 2019, the Chang'e‐4 (CE‐4) touched down on the Von Karman crater located inside the South Pole‐Aitken Basin, providing for the first time the opportunity for in situ measurements of the lunar regolith at the farside of the Moon. The CE‐4 ground penetrating radar reveals that fine‐grained regolith, coarse impact ejecta, and fractured bedrocks lie beneath the exploration path of the Yutu‐2 rover. The variations of regolith permittivity with depth and the radargrams indicate that the CE‐4 site has a fine‐grained regolith layer thickness of 11.1 m, which is about 1.3–3 times higher than the in situ measurement results at the Apollo and Chang'e‐3 (CE‐3) sites except for Apollo 16, possibly due to a faster weathering rate of ejecta deposits compared with coherent basalt substrates. The penetration depth of CE‐4 is about 2.85 times (in terms of round‐way delay) deeper than CE‐3, probably due to the differences in abundances of ilmenite and rocks in the regolith. Plain Language Summary: CE‐4 is the first craft in history to land on the lunar farside. Its rover is equipped with a ground‐penetrating radar (GPR), the same as the one mounted on the CE‐3 rover, which uses pulses of electromagnetic energy to reveal the subsurface structure and properties, especially useful to study the lunar soil layer ("regolith") that mantles most of the lunar surface. The results from the GPR show that the thickness of the regolith at the CE‐4 site is 1.3–3 times higher than the in situ measurements at the Apollo 11,12,14,15, 17, and CE‐3 sites even though the ages of the surfaces of Apollo 11 and Apollo 17 are thought to be comparable with that of the CE‐4 site. It implies a faster regolith growth speed at the CE‐4 site. The mineral mix of the surface materials at the CE‐4 site is different from that at the CE‐3: this results in less radar signal attenuation, thus increasing the detection limit up to the depth of 35 m, 2.85 times deeper than the CE‐3. Key Points: The LPR measurements at the CE‐4 landing site reveal that the shallow structure comprises of fine‐grained regolith, coarse impact ejecta, and fractured bedrocksThe CE‐4 landing site has a thicker regolith layer (~11 m) compared with the CE‐3, hinting at a longer weathering historyA lower abundance of ilmenite and rocks in the regolith at the CE‐4 site allows 2.85 times the penetration depth compared with CE‐3 site [ABSTRACT FROM AUTHOR]