Age of Luna 24 mare basalts based on crater studies

Boyce, J. M.; Schaber, G. G.; Dial, A. L.

doi:10.1038/265038a0

Cited by 16 publications

(7 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In the case of Mare Crisum and Mare Tranquillitatis regional phenomena can be responsible for the observed deviations. In particular, in both cases several consecutive magma flows have partially covered the population of small craters, affecting the observed cumulative distribution (Neukum & Horn 1976;Boyce et al 1977). Indeed the absolute radiometric ages derived from A11 samples (Mare Tranquillitatis), span from 3.5 to 3.85 Gyr, whereas the ages of the Luna 24 basalts (Mare Crisium) are clustered into at least three different peaks at 2.5, 3.3, 3.6 Gyr, respectively (Birck & Allègre 1978;Stöffler & Ryder 2001;Fernandes & Burgess 2005).…”

Section: Moon Crateringmentioning

confidence: 99%

A New Chronology for the Moon and Mercury

Marchi

Mottola

Cremonese

et al. 2009

The Astronomical Journal

170

241

View full text Add to dashboard Cite

In this paper we present a new method for dating the surface of the Moon, obtained by modeling the incoming flux of impactors and converting it into a size distribution of resulting craters. We compare the results from this model with the standard chronology for the Moon showing their similarities and discrepancies. In particular, we find indications of a non-constant impactor flux in the last 500 Myr and also discuss the implications of our findings for the Late Heavy Bombardment hypothesis. We also show the potential of our model for accurate dating of other inner Solar System bodies, by applying it to Mercury.

show abstract

Section: Moon Crateringmentioning

confidence: 99%

A New Chronology for the Moon and Mercury

Marchi

Mottola

Cremonese

et al. 2009

The Astronomical Journal

170

241

View full text Add to dashboard Cite

show abstract

“…The distances from the nearest highland sites approximate 50 km for Apollo 11, 25 km for Apollo 12, and 40 km for Luna 24 (R. L. Korotev, 2005, personal communication), the slopes for crater size frequency plots are À2.93, À2.86 and À3.0 [Shoemaker et al, 1970;Boyce et al, 1977] and the estimates of highland contamination are 28%, 46% and 10%, respectively [Korotev and Gillis, 2001; R. L. Korotev, 2005, personal communication]. Given these distances and an exponent 2.61 for ejecta thickness decay law, the model predicts 19.73% nonmare materials for Apollo 11 site, which is comparable to 28%; 42.11% nonmare materials for Apollo 12, which is close to 46%; and 11.96% nonmare materials for Luna 24 which is very close to 10%.…”

Section: Lateral Mixing Efficiencymentioning

confidence: 99%

On lateral mixing efficiency of lunar regolith

Mustard

2005

J. Geophys. Res.

View full text Add to dashboard Cite

[1] To reexamine the potential for lateral mixing over large distances (>100 km) by impact craters, a mathematical model utilizing the stable probability distribution is proposed for estimating lateral mixing efficiency on the Moon. The proposed model divides material mixing into shallow slope and steep slope regimes. Mixing in the shallow slope regime conforms to the condition that the exponent of the power law describing lunar crater size frequency is larger than the exponent of the power law describing the rim thickness plus 2; otherwise the mixing is called the steep slope regime. The model suggests that in the shallow slope regime, lateral mixing on the Moon is efficient enough to deliver 20-30% exotic components over distances greater than 100 km (e.g., highland material to the mare). The model indicates that lateral mixing conforming to the steep slope regime is not efficient if linear addition of ejecta deposits is assumed because in this regime, impact cratering is driven by small craters reworking lunar surface, and the addition of crater ejecta is an invalid assumption. If the result of the proposed model for the shallow slope regime is applied to regolith layers below the reworked zone, a significant number of ''exotic'' components is predicted.

show abstract

“…The basin is complex morphologically, suggesting that the basin was subjected to post-formation modification (Blewett et al 1995;Spudis, 2016, Yan et al 2010). Previous studies show a wide range of ages for the mare basalts here, ranging from 3.75 billion years to perhaps 2.5 billion years (Boyce and Johnson, 1977;Head et al, 1978;Hiesinger et al, 2011). The data from Chang'E (CE) Lunar Microwave Sounder (CELMS) permit a new perspective about the thermophysical features of the mare units in Mare Crisium.…”

Section: Introductionmentioning

confidence: 99%

“…Barsukov et al (1977) firstly studied the petrochemical and geochemical properties of the regolith and rocks based on the sample data from Luna 24, and the results indicated that the regolith here was monotonous in composition throughout the depth. Later, using the spectral data, Boyce and Johnson (1977) mapped the emplacement of geologic units within Mare Crisium and found three main units in the east central Mare Crisium. Head et al (1978) divided Mare Crisium into three Groups and an undivided area by studying the regional stratigraphy and geological history in Mare Crisium (Figure 1 (b)).…”

Section: Introductionmentioning

confidence: 99%

Potential Geological Significations of Crisium Basin Revealed by Ce-2 Celms Data

Meng

Wang

et al. 2018

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

View full text Add to dashboard Cite

ABSTRACT:Mare Crisium is one of the most prominent multi-ring basins on the nearside of the Moon. In this study, the regolith thermophysical features of Mare Crisium are studied with the CELMS data from CE-2 satellite. Several important results are as follows. Firstly, the current geological interpretation only by optical data is not enough, and a new geological perspective is provided. Secondly, the analysis of the low TB anomaly combined with the (FeO+TiO2) abundance and Rock abundance suggests a special unknown material in shallow layer of the Moon surface. At last, a new basaltic volcanism is presented for Crisium Basin. The study hints the potential significance of the CELMS data in understanding the geological units over the Moon surface.

show abstract

Age of Luna 24 mare basalts based on crater studies

Cited by 16 publications

References 6 publications

A New Chronology for the Moon and Mercury

A New Chronology for the Moon and Mercury

On lateral mixing efficiency of lunar regolith

Potential Geological Significations of Crisium Basin Revealed by Ce-2 Celms Data

Contact Info

Product

Resources

About