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Precambrian Era
Precambrian Era
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Precambrian
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The Precambrian Era
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WIKIPEDIA ARTICLE

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Precambrian Eon
4600–541 million years ago
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The Precambrian (or Pre-Cambrian, sometimes abbreviated , or Cryptozoic) is the earliest period of Earth's history, set before the current Phanerozoic Eon. The Precambrian is so named because it preceded the Cambrian, the first period of the Phanerozoic eon, which is named after Cambria, the Latinised name for Wales, where rocks from this age were first studied. The Precambrian accounts for 88% of the Earth's geologic time.

The Precambrian (colored green in the timeline figure) is a supereon that is subdivided into three eons (Hadean, Archean, Proterozoic) of the geologic time scale. It spans from the formation of Earth about 4.6 billion years ago (Ga) to the beginning of the Cambrian Period, about 541 million years ago (Ma), when hard-shelled creatures first appeared in abundance.

Overview[edit]

Relatively little is known about the Precambrian, despite it making up roughly seven-eighths of the Earth's history, and what is known has largely been discovered from the 1960s onwards. The Precambrian fossil record is poorer than that of the succeeding Phanerozoic, and fossils from that time (e.g. stromatolites) are of limited biostratigraphic use.[1] This is because many Precambrian rocks have been heavily metamorphosed, obscuring their origins, while others have been destroyed by erosion, or remain deeply buried beneath Phanerozoic strata.[1][2][3]

It is thought that the Earth coalesced from material in orbit around the Sun at roughly 4,543 Ma, and may have been struck by a very large (Mars-sized) planetesimal shortly after it formed, splitting off material that formed the Moon (see Giant impact hypothesis). A stable crust was apparently in place by 4,433 Ma, since zircon crystals from Western Australia have been dated at 4,404 ± 8 Ma.[4]

The term "Precambrian" is recognized by the International Commission on Stratigraphy as the only "supereon" in geologic time; it is so called because it includes the Hadean (~4.6-4 billion), Archean (4-2.5 billion), and Proterozoic (2.5 billion-541 million) eons. (There is only one other eon: the Phanerozoic, 541 million-present.)[5] "Precambrian" is still used by geologists and paleontologists for general discussions not requiring the more specific eon names.

Life forms[edit]

Landmass positions near the end of the Precambrian

A specific date for the origin of life has not been determined. Carbon found in 3.8-billion-year-old rocks (Archean eon) from islands off western Greenland may be of organic origin. Well-preserved microscopic fossils of bacteria older than 3.46 billion years have been found in Western Australia.[6] Probable fossils 100 million years older have been found in the same area. There is a fairly solid record of bacterial life throughout the remainder (Proterozoic eon) of the Precambrian.

Excluding a few contested reports of much older forms from North America and India, the first complex multicellular life forms seem to have appeared at roughly 1500 Ma, in the Neoproterozoic era of the Proterozoic eon. The oldest fossil evidence from that era of such complex life comes from the Lantian formation of the Ediacarian period, at least 580 million years ago. A very diverse collection of soft-bodied forms is found in a variety of locations worldwide and date to between 635 and 542 Ma. These are referred to as Ediacaran or Vendian biota. Hard-shelled creatures appeared toward the end of that time span, marking the beginning of the Phanerozoic era. By the middle of the following Cambrian period, a very diverse fauna is recorded in the Burgess Shale, including some which may represent stem groups of modern taxa. The explosion in diversity of lifeforms during the early Cambrian is called the Cambrian explosion of life.[7][8]

While land seems to have been devoid of plants and animals, cyanobacteria and other microbes formed prokaryotic mats that covered terrestrial areas.[9]

Planetary environment and the oxygen catastrophe[edit]

Weathered Precambrian pillow lava in the Temagami Greenstone Belt of the Canadian Shield

Evidence of the details of plate motions and other tectonic activity in the Precambrian has been poorly preserved. It is generally believed that small proto-continents existed prior to 4280 Ma, and that most of the Earth's landmasses collected into a single supercontinent around 1130 Ma. The supercontinent, known as Rodinia, broke up around 750 Ma. A number of glacial periods have been identified going as far back as the Huronian epoch, roughly 2400–2100 Ma. One of the best studied is the Sturtian-Varangian glaciation, around 850–635 Ma, which may have brought glacial conditions all the way to the equator, resulting in a "Snowball Earth".

The atmosphere of the early Earth is not well understood. Most geologists believe it was composed primarily of nitrogen, carbon dioxide, and other relatively inert gases, and was lacking in free oxygen. There is, however, evidence that an oxygen-rich atmosphere existed since the early Archean.[10]

At present, it is still believed that molecular oxygen was not a significant fraction of Earth's atmosphere until after photosynthetic life forms evolved and began to produce it in large quantities as a byproduct of their metabolism. This radical shift from a chemically inert to an oxidizing atmosphere caused an ecological crisis, sometimes called the oxygen catastrophe. At first, oxygen would have quickly combined with other elements in Earth's crust, primarily iron, removing it from the atmosphere. After the supply of oxidizable surfaces ran out, oxygen would have begun to accumulate in the atmosphere, and the modern high-oxygen atmosphere would have developed. Evidence for this lies in older rocks that contain massive banded iron formations, that were laid down as iron oxides.

Subdivisions[edit]

A terminology has evolved covering the early years of the Earth's existence, as radiometric dating has allowed real dates to be assigned to specific formations and features.[11] The Precambrian Supereon is divided into three eons: the Hadean (4600–4000 Ma), Archean (4000-2500 Ma) and Proterozoic (2500-541 Ma). See Timetable of the Precambrian.

  • Proterozoic: this eon refers to the time from the lower Cambrian boundary, 541 Ma, back through 2500 Ma. As originally used, it was a synonym for "Precambrian" and hence included everything prior to the Cambrian boundary. The Proterozoic eon is divided into three eras: the Neoproterozoic, Mesoproterozoic and Paleoproterozoic.
    • Neoproterozoic: The youngest geologic era of the Proterozoic Eon, from the Cambrian Period lower boundary (541 Ma) back to 1000 Ma. The Neoproterozoic corresponds to Precambrian Z rocks of older North American geology.
    • Mesoproterozoic: the middle era of the Proterozoic Eon, 1000-1600 Ma. Corresponds to "Precambrian Y" rocks of older North American geology.
    • Paleoproterozoic: oldest era of the Proterozoic Eon, 1600-2500 Ma. Corresponds to "Precambrian X" rocks of older North American geology.
  • Archean Eon: 2500-4000 Ma.
  • Hadean Eon: 4000–4600 Ma. This term was intended originally to cover the time before any preserved rocks were deposited, although some zircon crystals from about 4400 Ma demonstrate the existence of crust in the Hadean Eon. Other records from Hadean time come from the moon and meteorites.[12]

It has been proposed that the Precambrian should be divided into eons and eras that reflect stages of planetary evolution, rather than the current scheme based upon numerical ages. Such a system could rely on events in the stratigraphic record and be demarcated by GSSPs. The Precambrian could be divided into five "natural" eons, characterized as follows:[13]

  1. Accretion and differentiation: a period of planetary formation until giant Moon-forming impact event.
  2. Hadean: dominated by heavy bombardment from about 4.51 Ga (possibly including a Cool Early Earth period) to the end of the Late Heavy Bombardment period.
  3. Archean: a period defined by the first crustal formations (the Isua greenstone belt) until the deposition of banded iron formations due to increasing atmospheric oxygen content.
  4. Transition: a period of continued iron banded formation until the first continental red beds.
  5. Proterozoic: a period of modern plate tectonics until the first animals.

Precambrian super-continents[edit]

The movement of Earth's plates has caused the formation and break-up of continents over time, including occasional formation of a super-continent containing most or all of the landmass. The earliest known super-continent was Vaalbara. It formed from proto-continents and was a super-continent 3.636 billion years ago. Vaalbara broke up c. 2.845–2.803 Ga ago. The super-continent Kenorland was formed c. 2.72 Ga ago and then broke sometime after 2.45–2.1 Ga into the proto-continent cratons called Laurentia, Baltica, Australia, and Kalahari. The super-continent Columbia or Nuna formed 2.06–1.82 billion years ago and broke up about 1.5–1.35 billion years ago.[14][15][not in citation given] The super-continent Rodinia is thought to have formed about 1.13–1.071 billion years ago, to have embodied most or all of Earth's continents and to have broken up into eight continents around 750–600 million years ago.

See also[edit]

References[edit]

  1. ^ a b James Monroe and Reed Wicander, The Changing Earth, 2nd ed, (Belmont: Wadsworth Publishing Company, 1997), p. 492.
  2. ^ "Pamela J.W. Gore, "The Precambrian". Retrieved on 10/05/11". 
  3. ^ "The Precambrian Era". MIchigan State University. 
  4. ^ "Zircons are Forever". Retrieved 2007-04-28. 
  5. ^ International Commission on Stratigraphy. "International Chronostratigraphic Chart." Stratigraphy.org. Feb. 2017 (version 2017/02). <http://www.stratigraphy.org/index.php/ics-chart-timescale>.
  6. ^ Brun, Yves and Lawrence J. Shimkets, Prokaryotic development, ASM Press, Jan. 2000, p. 114 ISBN 978-1-55581-158-7
  7. ^ Fedonkin, Mikhail A.; James G. Gehling; Kathleen Grey; Guy M. Narbonne; Patricia Vickers-Rich (2008). The Rise of Animals: Evolution and Diversification of the Kingdom Animalia. JHU Press. ISBN 9780801886799. 
  8. ^ Dawkins, Richard; Yan Wong (2005). The Ancestor's Tale: A Pilgrimage to the Dawn of Evolution. Houghton Mifflin Harcourt. ISBN 9780618619160. 
  9. ^ Terrestrialization (Precambrian–Devonian)
  10. ^ Clemmey, Harry; Badham, Nick (1982). "Oxygen in the Precambrian Atmosphere". Geology. 10 (3): 141–146. Bibcode:1982Geo....10..141C. doi:10.1130/0091-7613(1982)10<141:OITPAA>2.0.CO;2. 
  11. ^ Geological Society of America's "2009 GSA Geologic Time Scale."
  12. ^ http://www.uwsp.edu/geo/faculty/hefferan/Geol106/CLASS3/hadean.htm
  13. ^ Bleeker, W. (2004) [2004]. "Toward a "natural" Precambrian time scale". In Felix M. Gradstein; James G. Ogg; Alan G. Smith. A Geologic Time Scale 2004. Cambridge University Press. ISBN 0-521-78673-8.  also available at Stratigraphy.org: Precambrian subcommission
  14. ^ Zhao, Guochun; Cawood, Peter A.; Wilde, Simon A.; Sun, M. (2002). "Review of global 2.1–1.8 Ga orogens: implications for a pre-Rodinia super-continent". Earth-Science Reviews. 59: 125–162. Bibcode:2002ESRv...59..125Z. doi:10.1016/S0012-8252(02)00073-9. 
  15. ^ Zhao, Guochun; Sun, M.; Wilde, Simon A.; Li, S.Z. (2004). "A Paleo-Mesoproterozoic super-continent: assembly, growth and breakup". Earth-Science Reviews. 67: 91–123. Bibcode:2004ESRv...67...91Z. doi:10.1016/j.earscirev.2004.02.003. 

Further reading[edit]

  • Valley, John W., William H. Peck, Elizabeth M. King (1999) Zircons Are Forever, The Outcrop for 1999, University of Wisconsin-Madison Wgeology.wisc.eduEvidence from detrital zircons for the existence of continental crust and oceans on the Earth 4.4 Gyr ago Accessed Jan. 10, 2006
  • Wilde, S. A.; Valley, J. W.; Peck, W. H.; Graham, C. M. (2001). "Evidence from detrital zircons for the existence of continental crust and oceans on the Earth 4.4 Gyr ago". Nature. 409 (6817): 175–178. PMID 11196637. doi:10.1038/35051550. 
  • Wyche, S.; Nelson, D. R.; Riganti, A. (2004). "4350–3130 Ma detrital zircons in the Southern Cross Granite–Greenstone Terrane, Western Australia: implications for the early evolution of the Yilgarn Craton". Australian Journal of Earth Sciences. 51 (1): 31–45. doi:10.1046/j.1400-0952.2003.01042.x. 

External links[edit]

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