The thermophysical properties of lunar regolith are crucial for lunar sciences and engineering. Here, we evaluate the thermophysical properties of lunar regolith between 75°N and 75°S from Diviner data by treating the radius of lunar regolith grains as a proxy. By the ground-truth median/average grain radius and Diviner data at several lunar landing sites, we recalibrate the reference rolling force for a grain radius of 0.475 μm as 0.9 ± 0.1 × 10−7 N. On a global scale, the estimated grain radius values focus mostly between 40 and 60 μm and show an average value of ∼55.3 μm. Some regions of Oceanus Procellarum, Mare Imbrium, and Mare Frigoris show abnormally large grain radius 80–100 μm, which are associated with the late high-Ti volcanism during 2.3–1.2 Ga within Procellarum KREEP Terrane. Mare Humorum is dated to be as old as 3.9 Ga, but still shows large grain radius values of ∼100 μm that are far greater than those in other contemporaneous mares. Such an anomaly may indicate a distinguished evolution for the local lunar regolith. For the surficial lunar regolith on the global scale, the contact component of thermal conductivity normalized to a temperature of 250 K varies mostly within 0.0008–0.0014 W (m K)−1, whereas the radiative component normalized to 250 K varies mostly within 0.002–0.004 W (m K)−1. The thickness of the topmost loosely packed layer is estimated as 0.02–0.07 m and tends to increase with the evolution of lunar regolith, which relates to the modification of packing style with the decrease of grain radius.
