Clark R. Chapman’s research while affiliated with Southwest Research Institute and other places

Lunar impact crater chronologies have been developed by combining carefully measured crater densities of lunar terrains with radiometric ages provided by returned samples. However, due to the sparse coverage of the samples during the last three billion years, this part of the chronologies is not well constrained. Lunar crater chronologies generally assume that the bombardment rate has been relatively constant during this epoch for all impactor sizes. Nevertheless, evidence has been gathering that this may not be the case for impactors larger than several hundred meters; however, there may be biases related to some of this evidence. The break-up of large asteroids in the Main Asteroid Belt to make asteroid families could be a source of a changing impact flux in the Earth-Moon system, especially when the families form near strong orbital resonances with the gas giants. In order to further explore the state of the impact flux from today to three billion years ago for impactors larger than ~5 km, we calculate crater retention model ages of 43 lunar craters 50 km and larger in diameter (D). Selected craters were initially suggested by United States Geological Survey geological maps of the Moon and Wilhems (1987) to have formed during the Copernican and Eratosthenian. We use the density of small (D < a few km) craters superposed on their floors, along with Model Production Function (MPF) lunar chronology (Marchi et al., 2009). For this purpose, we assume that the smaller impactors forming the superposed craters follow a constant flux as indicated by the MPF and supported by models of the dynamical evolution of the impactor population. We use the model ages as a proxy for the impact flux of larger impactors and test whether their distribution in time is consistent with a constant flux using two statistical analyses. Our results suggest that the flux of these larger impactors could be variable during the last three billion years, with hints of a relative increase in flux occurring ~2 billion years ago and a decrease in flux ~1 billion years ago. Thus, our results support the evidence that the impact flux has varied on the Moon for impactors over a few kilometers in diameter.

Observations of impact crater morphology can be used to gain insight into the geological history and evolution of a planet's surface. Image data from the Mariner 10 mission revealed the diversity of impact crater morphologies and degradational states on Mercury, leading to early studies that sought to establish a stratigraphic column for the planet, despite only acquiring image data for ~45% of the surface. In 2011, the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft entered orbit around Mercury, returning a high-resolution global image dataset that enables a robust analysis of crater morphology and degradation to be completed for the entirety of Mercury's surface. In this study, we conducted a visual classification of crater degradation according to initial crater morphology, and assigned a degradation state to all craters on Mercury ≥40 km in diameter. In our scheme, Class 1 craters are those that are heavily degraded, and Class 5 craters are very fresh with bright ray systems. We discuss the processes involved in crater degradation and erasure, and the challenges associated with applying crater degradation to derive the timing of geological events. We found that, based on the global spatial density of craters in each class, there appears to be a dearth of Class 1 craters within the intercrater plains, likely due to several ancient basin-sized impacts effectively obliterating a considerable portion of craters ≥40 km in diameter in this region. The crater degradation database we present here will serve as a useful tool for future analyses of Mercury's geological evolution.

Thanks to the NASA MESSENGER mission, our understanding of the planet Mercury has never been greater, and the dual-spacecraft ESA–JAXA BepiColombo mission promises further breakthroughs in Mercury science. Yet there is only so much that can be accomplished from orbit. Here, we detail outstanding questions related to several aspects of Mercury’s character and evolution that can be addressed either more fully, or uniquely, by a landed mission. We discuss major outstanding questions of Mercury science that encompass five categories, and suggest how they might be addressed. Those categories include: ▪ the planet’s geochemical makeup; ▪ its interior structure; ▪ the geological evolution of Mercury; ▪ present-day processes at work there; and ▪ the planet’s polar volatile inventory.

We analyze a comprehensive set of our adaptive optics (AO) images taken at the 10 m W. M. Keck telescope and the 8 m Gemini telescope to derive values for the size, shape, and rotational pole of asteroid (16) Psyche. Our fit of a large number of AO images, spanning 14 years and covering a range of viewing geometries, allows a well-constrained model that yields small uncertainties in all measured and derived parameters, including triaxial ellipsoid dimensions, rotational pole, volume, and density. We find a best fit set of triaxial ellipsoid diameters of (a,b,c) = (274 ± 9, 231 ± 7, 176 ± 7) km, with an average diameter of 223 ± 7 km. Continuing the literature review of Carry (2012), we find a new mass for Psyche of 2.43 ± 0.35 × 10¹⁹ kg that, with the volume from our size, leads to a density estimate 4.16 ± 0.64 g/cm³. The largest contribution to the uncertainty in the density, however, still comes from the uncertainty in the mass, not our volume. Psyche’s M classification, combined with its high radar albedo, suggests at least a surface metallic composition. If Psyche is composed of pure nickel-iron, the density we derive implies a macro-porosity of 47%, suggesting that it may be an exposed, disrupted, and reassembled core of a Vesta-like planetesimal. The rotational pole position (critical for planning spacecraft mission operations) that we find is consistent with others, but with a reduced uncertainty: [RA;Dec]=[32°;+5°] or Ecliptic [λ; δ]=[32∘;−8∘] with an uncertainty radius of 3°. Our results provide independent measurements of fundamental parameters for this M-type asteroid, and demonstrate that the parameters are well determined by all techniques, including setting the prime meridian over the longest principal axis. The 5.00 year orbital period of Psyche produces only four distinct opposition geometries, suggesting that observations before the arrival of Psyche Mission in 2030 should perhaps emphasize observations away from opposition, although the penalty then would be that the asteroid will be fainter and further than at opposition.

Impact crater populations help us to understand solar system dynamics, planetary surface histories, and surface modification processes. A single previous effort to standardize how crater data are displayed in graphs, tables, and archives was in a 1978 NASA report by the Crater Analysis Techniques Working Group, published in 1979 in Icarus. The report had a significant lasting effect, but later decades brought major advances in statistical and computer sciences while the crater field has remained fairly stagnant. In this new work, we revisit the fundamental techniques for displaying and analyzing crater population data and demonstrate better statistical methods that can be used. Specifically, we address (1) how crater size-frequency distributions (SFDs) are constructed, (2) how error bars are assigned to SFDs, and (3) how SFDs are fit to power-laws and other models. We show how the new methods yield results similar to those of previous techniques in that the SFDs have familiar shapes but better account for multiple sources of uncertainty. We also recommend graphic, display, and archiving methods that reflect computers’ capabilities and fulfill NASA's current requirements for Data Management Plans.

Following an approach similar to that used for the Moon, Mercury's surface units were subdivided into five time-stratigraphic systems based on geologic mapping using Mariner 10 images. The absolute time scale originally suggested for the time periods associated with these systems was based on the assumption that the lunar impact-flux history applied to Mercury. However, we find that the duration and onset of corresponding periods in the stratigraphic sequences on Mercury and the Moon are not the same. Using high-resolution and multi-band image data obtained by the MErcury Surface, Space ENviroment, GEochemistry, and Ranging (MESSENGER) spacecraft, we identify and catalog and fresh impact craters interpreted to have formed during Mercury's two most recent periods, the Mansurian and Kuiperian. The densities of the inferred Kuiperian- and Mansurian-aged crater populations are used to estimate new limits for the age boundaries of these time intervals. Results suggest that both the Mansurian and Kuiperian periods began more recently and extended for significantly shorter durations of time than previously suggested. The Kuiperian is estimated to have initiated as recently as ~280 ± 60 Ma and the Mansurian as recently as ~1.7 ± 0.2 Ga.

Large tectonic landforms on the surface of Mercury, consistent with significant contraction of the planet, were revealed by the flybys of Mariner 10 in the mid-1970s. The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission confirmed that the planet's past 4 billion years of tectonic history have been dominated by contraction expressed by lobate fault scarps that are hundreds of kilometres long. Here we report the discovery of small thrust fault scarps in images from the low-altitude campaign at the end of the MESSENGER mission that are orders of magnitude smaller than the large-scale lobate scarps. These small scarps have tens of metres of relief, are only kilometres in length and are comparable in scale to small young scarps on the Moon. Their small-scale, pristine appearance, crosscutting of impact craters and association with small graben all indicate an age of less than 50 Myr. We propose that these scarps are the smallest members of a continuum in scale of thrust fault scarps on Mercury. The young age of the small scarps, along with evidence for recent activity on large-scale scarps, suggests that Mercury is tectonically active today and implies a prolonged slow cooling of the planet's interior.

Galileo observations in the UV, visible, and infrared uniquely characterize the luminous phenomena associated primarily with the early stages of the impacts of SL9 fragments—the bolide and fireball phases—because of the spacecraft's direct view of the impact sites. The single luminous events, typically 1 min in duration at near-IR wavelengths, are interpreted as initial bolide flashes in the stratosphere followed immediately by development of a fireball above the ammonia clouds, which subsequently rises, expands, and cools from ∼ 8000 K to ∼ 1000 K over the first minute. The brightnesses of the bolide phases were remarkably similar for disparate events, including L and N, which were among the biggest and smallest of the impacts as classified by Earth-based phenomena. Subsequent fireball brightnesses differ much more, suggesting that the similar-sized fragments were near the threshold for creating fireballs and large dark features on Jupiter's face. Both bolides and fireballs were much dimmer than had been predicted before the impacts, implying that impactor masses were small (∼0.5km diameter). Galileo data clarify the physical interpretation of the “first precursor,” as observed from Earth: it probably represents a massive meteor storm accompanying the main fragment, peaking ∼10s before the fragment penetrates to the tropopause; hints of behind-the-limb luminous phenomena, recorded from Earth immediately following the peak of the first precursor, may be due to reflection of the late bolide/early fireball stages from comet debris very high in Jupiter's atmosphere.