Re-examining the main asteroid belt as the primary source of ancient lunar craters

• Published in: Icarus (New York, N.Y. 1962) Vol. 247; pp. 172 - 190
• Main Authors: Minton, David A., Richardson, James E., Fassett, Caleb I.
• Format: Journal Article
• Language: English
• Published: Elsevier Inc 01.02.2015
• Subjects: Asteroid belts; Asteroids; Basins; Bombardment; Computer simulation; Cratering; Craters; Highlands; Impactors; Moon; Moon, surface; Cratering; Moon, surface; Asteroids
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2014.10.018

•The modern main asteroid belt SFD is a poor model for lunar highlands impactors.•The lunar highlands impactors had a larger number of small objects than the MAB.•A new Monte Carlo cratering code has been calibrated with a human crater counter. It has been hypothesized that the impactors that created the majority of the observable craters on the ancient lunar highlands were derived from the main asteroid belt in such a way that preserved their size–frequency distribution (Strom, R.G., Malhotra, R., Ito, T., Yoshida, F., Kring, D.A. [2005]. Science 309, 1847–1850). A more limited version of this hypothesis, dubbed the E-belt hypothesis, postulates that a destabilized contiguous inner extension of the main asteroid belt produced a bombardment limited to those craters younger than Nectaris basin (Bottke, W.F., Vokrouhlický, D., Minton, D., Nesvorný, D., Morbidelli, A., Brasser, R., Simonson, B., Levison, H.F. [2012]. Nature 485, 78–81). We investigate these hypotheses with a Monte Carlo code called the Cratered Terrain Evolution Model (CTEM), which models the topography of a terrain that has experienced bombardment due to an input impactor population. We detail our effort to calibrate the code with a human crater counter. We also take advantage of recent advances in understanding the scaling relationships between impactor size (Di) and final crater size (Dc) for basin-sized impact craters (Dc>300km) in order to use large impact basins as a constraint on the ancient impactor population of the Moon. We find that matching the observed number of lunar highlands craters with Dc≃100km requires that the total number of impacting asteroids with Di>10km be no fewer than 4×10-6km-2. However, this required mass of impactors has <1% chance of producing only a single basin larger than the ∼1200km Imbrium basin; instead, these simulations are likely to produce more large basins than are observed on the Moon. This difficulty in reproducing the lunar highlands cratering record with a main asteroid belt SFD arises because the main belt is relatively abundant in the objects that produce these “megabasins” that are larger than Imbrium. We also find that the main asteroid belt SFD has <16% chance of producing Nectarian densities of Dc>64km craters while not producing a crater larger than Imbrium, as required by the E-belt hypothesis. These results suggest that the lunar highlands were unlikely to have been bombarded by a population whose size–frequency distribution resembles that of the currently observed main asteroid belt. We suggest that the population of impactors that cratered the lunar highlands had a somewhat similar size–frequency distribution as the modern main asteroid belt, reflecting a similar rocky composition and collisional history, but had a smaller ratio of objects capable of producing megabasins compared to objects capable of producing ∼100km craters. We estimate that the impactor population required to match the lunar highlands had N>5.5km/N>70km≃630, while the modern main asteroid belt ratio is N>5.5km/N>70km≃100.