Geological mapping and chronology of lunar landing sites: Apollo 11

Iqbal, W.; Hiesinger, H.; Bogert, C. H. van der

doi:10.1016/j.icarus.2019.06.020

Cited by 15 publications

(15 citation statements)

References 38 publications

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“…The Apollo 11 landing site is located in the south of Mare Tranquillitatis (Figure 3a). A recent detailed geological study based on multispectrum, topography and albedo shows that the landing region is relatively uniform (Iqbal et al, 2019; see also Text S1 in Supporting Information S1). Observations from the in situ passive seismic experiment (PSE) suggested a regolith thickness of 4.4 ± 1.0 m (Nakamura et al, 1975).…”

Section: Applications To the Apollo 11 And 14 Landing Sitesmentioning

confidence: 99%

Effect of Topographic Degradation on Small Lunar Craters: Implications for Regolith Thickness Estimation

Yang

et al. 2021

Geophysical Research Letters

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The continuous impacts of large and small meteoroids with the lunar surface over billions of years have created a global fine-grained regolith layer on the Moon. The nature, structure, stratigraphy, and history of regolith not only preserve key information about the Moon's geology, inner solar system impact flux, and solar wind history, but also are important for future in situ explorations (e.g., Fa & Wieczorek, 2012;McKay et al., 1991;Wilcox et al., 2005). Regolith formation is a self-limiting process and can be divided roughly into two stages. Shortly after a solid surface is formed, there is no or little regolith, and both large and small impacts can excavate bedrock and produce new regolith. As time goes on, regolith becomes thicker, and thus only progressively larger impacts can penetrate through the regolith layer and produce new regolith materials. Small impacts only rework the regolith layer already present at this stage. Depending on whether or not regolith layer can be penetrated through (i.e., regolith thickness), small impacts can produce four typical classes of craters with different morphologies: normal, central mound, flat-bottomed, and concentric (Figure S1 in Supporting Information S1; Gault et al., 1966;

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Section: Applications To the Apollo 11 And 14 Landing Sitesmentioning

confidence: 99%

Effect of Topographic Degradation on Small Lunar Craters: Implications for Regolith Thickness Estimation

Yang

et al. 2021

Geophysical Research Letters

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“…Therefore, such data can be used to retrieve the geological age of the stars [3], analyze the tectonic history of the lead [4], and explore the existence of iced water [5]. In addition, it can be used for autonomous navigation [6], landing site selection [7], base selection, and other missions of deep space probs.…”

Section: Introductionmentioning

confidence: 99%

Split-Attention Networks with Self-Calibrated Convolution for Moon Impact Crater Detection from Multi-Source Data

et al. 2021

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Impact craters are the most prominent features on the surface of the Moon, Mars, and Mercury. They play an essential role in constructing lunar bases, the dating of Mars and Mercury, and the surface exploration of other celestial bodies. The traditional crater detection algorithms (CDA) are mainly based on manual interpretation which is combined with classical image processing techniques. The traditional CDAs are, however, inefficient for detecting smaller or overlapped impact craters. In this paper, we propose a Split-Attention Networks with Self-Calibrated Convolution (SCNeSt) architecture, in which the channel-wise attention with multi-path representation and self-calibrated convolutions can generate more prosperous and more discriminative feature representations. The algorithm first extracts the crater feature model under the well-known target detection R-FCN network framework. The trained models are then applied to detecting the impact craters on Mercury and Mars using the transfer learning method. In the lunar impact crater detection experiment, we managed to extract a total of 157,389 impact craters with diameters between 0.6 and 860 km. Our proposed model outperforms the ResNet, ResNeXt, ScNet, and ResNeSt models in terms of recall rate and accuracy is more efficient than that other residual network models. Without training for Mars and Mercury remote sensing data, our model can also identify craters of different scales and demonstrates outstanding robustness and transferability.

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“…The calibration for this method, which allows converting crater densities (i.e., crater size–frequency distributions [CSFDs]) to absolute model ages, is based on returned Apollo and Luna samples that can be linked to a geological unit (e.g., a lava flow) or an impact basin/crater for which absolute radiometric or cosmic ray exposure (CRE) ages have been determined (Fig. 1) (e.g., Hiesinger et al., 2012; Iqbal et al., 2019; Neukum, 1983; Neukum et al., 2001; Robbins, 2014). For the last 1 Ga, the lunar cratering chronology function is constrained by the crater densities on the ejecta blankets surrounding Copernicus, Tycho, North Ray, and Cone craters.…”

Section: Introductionmentioning

confidence: 99%

“…Lunar cratering chronology (modified from Hiesinger et al., 2012; Iqbal et al., 2019; Neukum, 1983; Neukum et al., 2001). Cumulative number of craters ≥1 km in diameter per km 2 as a function of the age of dated lunar surfaces.…”

Section: Introductionmentioning

confidence: 99%

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Noble gas exposure ages of samples from Cone and North Ray craters: Implications for the recent lunar cratering chronology

Füri

Zimmermann

Hiesinger

2021

Meteorit & Planetary Scien

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Cosmic ray exposure (CRE) ages of rocks that were ejected by the impacts that created Cone and North Ray craters provide two crucial calibration points at <100 Ma for the lunar cratering chronology function, which relates the crater density of geological units on the Moon to their absolute age. To reassess the formation ages of these two craters, we determine here the accumulated abundances of “cosmogenic” noble gas nuclides (3Hecosm, 21Necosm, 38Arcosm), as well as the corresponding CRE ages, in six Apollo 14 rocks (i.e., one breccia and five basalts) and two Apollo 16 anorthosites that were collected near the rims of Cone and North Ray craters, respectively. Although noble gas concentrations allow CRE ages to be derived, the calculated 21Ne and 38Ar exposure ages of a given sample cover a significant range of values because published empirical or theoretical production rates of cosmogenic nuclides are highly variable. Nonetheless, it is evident that mare basalts 14053 and 14072 as well as breccia 14068, which were collected near the rim of Cone crater, were exposed at the lunar surface more recently than the three KREEP basalts (14073, 14077, 14078) collected farther away. The 38Ar exposure ages of anorthosites 67075 and 67955 from North Ray crater slightly exceed those of samples 14053, 14068, and 14072. These results confirm that Cone crater is younger than North Ray crater. However, the formation ages of Cone and North Ray craters have larger uncertainties than previously acknowledged. This implies that the uncertainties of noble gas exposure ages should be taken into account when remotely dating young surfaces on the Moon and on other planetary bodies in the solar system.

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Geological mapping and chronology of lunar landing sites: Apollo 11

Abstract: Crater size-frequency distribution (CSFDs) measurements allow the derivation of absolute model ages (AMAs) for geological units across various terrestrial bodies in the Solar System based on body-specific adjustments to the lunar chronology (e.g.

Cited by 15 publications

References 38 publications

Effect of Topographic Degradation on Small Lunar Craters: Implications for Regolith Thickness Estimation

Effect of Topographic Degradation on Small Lunar Craters: Implications for Regolith Thickness Estimation

Split-Attention Networks with Self-Calibrated Convolution for Moon Impact Crater Detection from Multi-Source Data

Noble gas exposure ages of samples from Cone and North Ray craters: Implications for the recent lunar cratering chronology

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