Evolution of a habitable planet

James Kasting, Kirschvink Joseph

Research output: Chapter in Book/Report/Conference proceedingChapter

Abstract

We saw in the previous chapter that Earth developed a climate that supported liquid water at its surface very early in its history, probably within the first few hundred million years. That was good for life, of course, because all life that we know about on Earth requires liquid water at least episodically. There are good chemical reasons for thinking that this requirement might be universal, some of which were discussed earlier in this volume. Here we are concerned with a somewhat later stage in Earth's history, starting from when the rock record begins, around 3.8–4 billion years ago, or 3.8–4 Gyr ago, and continuing on until the rise of atmospheric oxygen, around 2.3 Gyr ago. This time interval overlaps almost precisely with the geologic time period called the Archean Eon. Although not formally defined as such, the beginning of the Archean corresponds with the beginning of the rock record, as marked by the oldest dated fragments of continental crust at Earth's surface. We know that Earth had older rocks, based on crystals of the mineral, zircon, which survive today as sand grains in mid-Archean quartzites from Western Australia, and can be dated as far back as 4.4 Gyr ago (Valley et al. 2002). Defining the end of Archean time to be precisely 2.5 Gyr ago was a somewhat arbitrary decision of the geological community: at about this time, the dominant type of sedimentary basin switches from the granite-greenstone belt configuration (dominated by ultramafic, magnesium-rich volcanics and chemically immature sedimentary rocks) to basins controlled by thermal subsidence along passive margins. This switch in rock types may or may not have influenced the rise of O2, as discussed later in this chapter. We will henceforth use the term “Archean” to refer to the time period preceding the rise of O2, recognizing that astrobiological and geological terminologies have slightly different meanings.

Original languageEnglish (US)
Title of host publicationFrontiers of Astrobiology
PublisherCambridge University Press
Pages115-131
Number of pages17
ISBN (Electronic)9780511902574
ISBN (Print)9781107006416
DOIs
StatePublished - Jan 1 2009

Fingerprint

planets
rocks
switches
histories
terminology
sedimentary rocks
subsidence
Earth surface
granite
liquids
water
sands
climate
magnesium
volcanology
margins
crusts
minerals
fragments
intervals

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cite this

Kasting, J., & Joseph, K. (2009). Evolution of a habitable planet. In Frontiers of Astrobiology (pp. 115-131). Cambridge University Press. https://doi.org/10.1017/CBO9780511902574.010
Kasting, James ; Joseph, Kirschvink. / Evolution of a habitable planet. Frontiers of Astrobiology. Cambridge University Press, 2009. pp. 115-131
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Kasting, J & Joseph, K 2009, Evolution of a habitable planet. in Frontiers of Astrobiology. Cambridge University Press, pp. 115-131. https://doi.org/10.1017/CBO9780511902574.010

Evolution of a habitable planet. / Kasting, James; Joseph, Kirschvink.

Frontiers of Astrobiology. Cambridge University Press, 2009. p. 115-131.

Research output: Chapter in Book/Report/Conference proceedingChapter

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Kasting J, Joseph K. Evolution of a habitable planet. In Frontiers of Astrobiology. Cambridge University Press. 2009. p. 115-131 https://doi.org/10.1017/CBO9780511902574.010