Lunar geologic timescale
Template:Lunar-geo-time The lunar geologic timescale (or selenologic timescale) divides the history of Earth's moon into five generally recognized geologic periods: the Copernican, Eratosthenian, Imbrian (upper and lower), Nectarian, and Pre-Nectarian. The boundaries of this time scale are related to large impact events that have modified the lunar surface, changes in crater morphology that occur though time, and the size-frequency distribution of craters superposed on geologic units. The absolute ages for these periods have been constrained by radiometric dating of samples obtained from the lunar surface. However, as a result of the difficulty of determining which geologic unit any given rock on the lunar surface is derived from, there is still much debate concerning the ages of certain key events.
Lunar stratigraphy
The primary geologic processes that have modified the lunar surface are impact cratering and volcanism, and by using standard stratigraphic principles[1] (such as the law of superposition) it is possible to order these geologic events in time. At one time, it was thought that the mare basalts might represent a single stratigraphic unit with a unique age, but it is now recognized that mare volcanism was an ongoing process, beginning as early as 4.2 Ga[2] and continuing to perhaps as late as 1.2 Ga (1 Ga = 1 billion years ago).[3] Impact events are by far the most useful for defining a lunar stratigraphy as they are numerous and form in a geologic instant.[4] The continued effects of impact cratering over long periods of time modify the morphology of lunar landforms in a quantitative way, and the state of erosion of a landform can also be used to assign a relative age.
The lunar geologic time scale has been divided into five periods (Pre-Nectarian, Nectarian, Imbrian, Eratosthenian, and Copernican) with one of these (the Imbrian) being subdived into two epochs. These divisions of geologic time are based on the recognition of convenient geomorphologic markers, and as such, they should not be taken to imply that any fundamental changes in geologic processes have occurred at these boundaries. The Moon is unique in the Solar System in that it is the only body (other than the Earth) for which we possess rock samples with a known geologic context. By correlating the ages of samples obtained from the Apollo missions to known geologic units, it has been possible to assign absolute ages to some of these geologic periods. The timeline below represents one such attempt, but it is important to note (as is discussed below) that some of the ages are either uncertain, or disputed. In many lunar highland regions, it is not possible to distinguish between Nectarian and Pre-Nectarian materials, and these deposits are sometimes labeled as just Pre-Imbrian.
Pre-Nectarian
The Pre-Nectarian period is defined from the point at which the lunar crust formed, to the time of the Nectaris impact event. Nectaris is a multi-ring impact basin that formed on the near side of the Moon, and its ejecta blanket serves as a useful stratigraphic marker. 30 impact basins from this period are recognized, the oldest of which is the South Pole-Aitken basin. This geologic period has been informally subdivided into the Cryptic and Basin Groups 1-9,[1] but these divisions are not used on any geologic maps.
Nectarian
The Nectarian period encompasses all events that occurred between the formation of the Nectaris and Imbrium impact basins. 12 multi-ring impact basins are recognized in the Nectarian period, including the Serenitatis and Crisium basins. One of the scientific objectives of the Apollo 16 mission was to date material excavated by the Nectaris impact basin. Nevertheless, the age of the Nectaris basin is somewhat contentious, with the most frequently cited numbers being 3.92 Ga, and less frequently 3.85 Ga. Recently, it has been suggested that the Nectaris basin could be, in fact, much older at ~4.1 Ga.[5]
Imbrian
The Imbrian period has been subdivided into upper and lower epochs. The Lower Imbrian is defined as the period of time between the formation of the Imbrium and Orientale impact basins. The Imbrium basin is believed to have formed at 3.85 Ga, though a minority opinion places this event at 3.77 Ga. The Schrödinger basin is the only other multi-ring basin that is Lower Imbrian in age, and no large multi-ring basins formed after this epoch.
The Upper Imbrian is defined as the time between the formation of the Orientale basin, and the time at which craters of a certain size (DL) have been obliterated by erosional processes. The age of the Orientale basin has not been directly determined, though it must be older than 3.72 Ga (based on Upper Imbrian ages of mare basalts) and could be as old as 3.84 Ga based on the size-frequency distributions of craters superposed on Orientale ejecta. About two-thirds of the Moon's mare basalts erupted within the Upper Imbrian, with many of these lavas filling the depressions associated with older impact basins.
Eratosthenian
The base of the Eratosthenian period is defined by the time at which craters on a geologic unit of a certain size DL have been almost completely obliterated by erosional processes. The principle erosional agent on the Moon is impact cratering itself, though seismic modification could play a minor role as well. The absolute age of this boundary is not well defined, but is commonly quoted as being near 3.2 Ga. The younger boundary of this period is defined based on the recognition that freshly excavated materials on the lunar surface are generally "bright" and that they become darker over time as a result of space weathering processes. Operationally, this period was originally defined as the time at which impact craters "lost" their bright ray systems. This definition, however, has recently been subjected to some criticism as some crater rays are bright for compositional reasons that are unrelated to the amount of space weathering they have incurred. In particular, if the ejecta from a crater formed in the highlands (which is composed of bright anorthositic materials) is deposited on the low albedo mare, it will remain bright even after being space weathered.
Copernican
The Copernican period is the youngest geologic period of the Moon. Originally, the presence of a bright ray system surrounding an impact crater was used to define Copernican units, but as mentioned above, this is complicated by the presence of compositional ray systems. The base of the Copernican period does not correspond to the formation of the Copernicus impact crater. The age of the base of the Copernican is not well constrained, but a commonly quoted number is 1.1 Ga. The Copernican extends until the present day.
Relationship to Earth's geologic time scale
The divisions of the lunar geologic time scale are based on the recognition of a few convenient geomorphologic markers. While these divisions are extremely useful for ordering geologic events in a relative manner, it is important to realize that the boundaries do not imply any fundamental change of geologic processes. Furthermore, as the oldest geologic periods of the Moon are based exclusively on the times of individual impact events (in particular, Nectaris, Imbrium, and Orientale), these punctual events will most likely not correspond to any specific geologic event on the other terrestrial planets, such as Mercury, Venus, Earth, or Mars.
Nevertheless, at least one notable scientific work[6] has advocated using the lunar geologic time scale to subdivide the Hadean eon of Earth's Geologic timescale (it should be noted that the Hadean eon is not officially recognized). In particular, it is sometimes found that the Hadean is subdivided into the Cryptic, Basin Groups 1-9, Nectarian, and Lower Imbrian. This notation is not entirely consistent with the above lunar geologic time scale in that the Cryptic and Basin Groups 1-9 (both of which are only informal terms that are not used in geologic maps) comprise the Pre-Nectarian period.
See also
- Crater counting
- Geology of the Moon
- Geologic time scale (Earth)
- Impact crater
- Late Heavy Bombardment
References
Cited references
- ^ a b Don Wilhelms (1987). Geologic History of the Moon. U.S. Geological Survey Professional Paper 1348.
{{cite book}}: External link in|title= - ^ James Papike, Grahm Ryder, and Charles Shearer (1998). "Lunar Samples". Reviews in Mineralogy and Geochemistry. 36: 5.1–5.234.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ H. Hiesinger, J. W. Head, U. Wolf, R. Jaumanm, and G. Neukum (2003). "Ages and stratigraphy of mare basalts in Oceanus Procellarum, Mare Numbium, Mare Cognitum, and Mare Insularum". J. Geophys. Res. 108: doi:10.1029/2002JE001985.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ D. Stöffler and G. Ryder (2001). "Stratigraphy and isotope ages of lunar geologic units: chronological standards for the inner solar system". Space Sci. Rev. 96: 9–54.
- ^ R. Korotev, J. Gillis, L. Haskin, and B. Jolliff (2002). "On the age of the Nectaris basin". Workshop on Moon Beyond: abstract 3029.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ W. Harland, R. Armstrong, A. Cox, L. Craig, A. Smith, D. Smith (1990). A Geologic time scale 1989. Cambridge University Press.
{{cite book}}: CS1 maint: multiple names: authors list (link)
General references
- Linda Martel (September 28, 2004). "Lunar Crater Rays Point to a New Lunar Time Scale".