Abstract
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.
Highlights
The heavily-cratered highlands of the Moon are uniquely suited as a terrain for studying the early bombardment history of the inner solar system
Each pixel contains a variety of data, one of which is the current elevation at that location, allowing the construction of a Digital Elevation Model (DEM) of the surface
Because including estimates of the number of large lunar impact basins is a critical component of our present work, in Subsection 2.2 we describe how we incorporated recently published scaling relationships for lunar basins based on computer hydrocode modeling into Cratered Terrain Evolution Model (CTEM)
Summary
The heavily-cratered highlands of the Moon are uniquely suited as a terrain for studying the early bombardment history of the inner solar system. Little post-bombardment geological processing has modified highlands craters over the ∼ 3.5 Gy since the majority of them formed. The combination of impactdominated geology and an abundant and diverse sample record means that the lunar cratering record has been the primary source for absolute-age crater chronology systems. It is the best record currently available for testing models for the bombardment history of the inner solar system
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