Faint young Sun paradox

The faint young Sun paradox describes the apparent contradiction between observations of liquid water early in Earth's history and the astrophysical expectation that the Sun's output would be only 70 percent as intense during that epoch as it is during the modern epoch. The issue was raised by astronomers Carl Sagan and George Mullen in 1972.[1] Explanations of this paradox have taken into account greenhouse effects, astrophysical influences, or a combination of the two.

Early solar output

Early in Earth's history, the Sun's output would have been only 70 percent as intense as it is during the modern epoch. In the environmental conditions existing at that time, this solar output would have been insufficient to maintain a liquid ocean. Astronomers Carl Sagan and George Mullen pointed out in 1972 that this is contrary to the geological and paleontological evidence.[1]

According to the Standard Solar Model, stars similar to the Sun should gradually brighten over their main sequence lifetime due to contraction of the stellar core caused by fusion.[2] However, with the predicted solar luminosity 4 billion (4 × 109) years ago and with greenhouse gas concentrations the same as are current for the modern Earth, any liquid water exposed to the surface would freeze. However, the geological record shows a continually relatively warm surface in the full early temperature record of Earth, with the exception of a cold phase, the Huronian glaciation, about 2.4 to 2.1 billion years ago. Water-related sediments have been found dating to as early as 3.8 billion years ago.[3] Hints of early life forms have been dated from as early as 3.5 billion years,[4] and the basic carbon isotopy is very much in line with what is found today.[5] A regular alternation between ice ages and warm periods is only found occurring in the period since one billion years ago.

Greenhouse hypothesis

When it first formed, Earth's atmosphere may have contained more greenhouse gases. Carbon dioxide concentrations may have been higher, with estimated partial pressure as large as 1,000 kPa (10 bar), because there was no bacterial photosynthesis to reduce the gas to carbon and oxygen. Methane, a very active greenhouse gas that reacts with oxygen to produce carbon dioxide and water vapor, may have been more prevalent as well, with a mixing ratio of 10−4 (100 parts per million by volume).[6][7]

Based on a study of geological sulfur isotopes, in 2009 a group of scientists including Yuichiro Ueno from the University of Tokyo proposed that carbonyl sulfide (OCS) was present in the Archean atmosphere. Carbonyl sulfide is an efficient greenhouse gas and the scientists estimate that the additional greenhouse effect would have been sufficient to prevent Earth from freezing over.[8]

Based on an "analysis of nitrogen and argon isotopes in fluid inclusions trapped in 3.0- to 3.5-billion-year-old hydrothermal quartz" a 2013 paper concludes that "dinitrogen did not play a significant role in the thermal budget of the ancient Earth and that the Archean partial pressure of CO2 was probably lower than 0.7 bar".[9] Burgess, one of the authors states "The amount of nitrogen in the atmosphere was too low to enhance the greenhouse effect of carbon dioxide sufficiently to warm the planet. However, our results did give a higher than expected pressure reading for carbon dioxide – at odds with the estimates based on fossil soils – which could be high enough to counteract the effects of the faint young Sun and will require further investigation."[10]

Following the initial accretion of the continents after about 1 billion years,[11] geo-botanist Heinrich Walter and others contend that a non-biological version of the carbon cycle provided a negative temperature feedback. The carbon dioxide in the atmosphere dissolved in liquid water and combined with metal ions derived from silicate weathering to produce carbonates. During ice age periods, this part of the cycle would shut down. Volcanic carbon emissions would then restart a warming cycle due to the greenhouse effect.[12][13]

According to the Snowball Earth hypothesis, there may have been a number of periods when Earth's oceans froze over completely. The most recent such period may have been about 630 million years ago.[14] Afterwards, the Cambrian explosion of new multicellular life forms started.

Greater radiogenic heat

The radiogenic heat from the decay of 5 isotopes affecting Earth's internal heat budget over time, in the past the contribution from 40K and 235U was much higher and thus the overall radiogenic heat output was higher.

In the past, the geothermal release of decay heat, emitted from the decay of the isotopes potassium-40, uranium-235 and uranium-238 was considerably greater than it is today.[15] The figure to the right shows that the isotope ratio between U-238 to U-235 was also considerably different than it is today, with the ratio essentially equivalent to that of modern low-enriched uranium. Therefore, natural uranium ore bodies, if present, would have been capable of supporting natural nuclear fission reactors with common light water as its moderator. Any attempts to explain the paradox must therefore factor in both radiogenic contributions, both from decay heat and from any potential natural nuclear fission reactors.

Greater tidal heating

The Moon was much closer to Earth billions of years ago,[16] and therefore produced considerably more tidal heating.[17]

Alternatives

Phanerozoic Climate Change

A minority view, propounded by the Israeli-American physicist Nir Shaviv, uses climatological influences of solar wind, combined with a hypothesis of Danish physicist Henrik Svensmark for a cooling effect of cosmic rays, to explain the paradox.[18] According to Shaviv, the early Sun had emitted a stronger solar wind that produced a protective effect against cosmic rays. In that early age, a moderate greenhouse effect comparable to today's would have been sufficient to explain an ice-free Earth. Evidence for a more active early Sun has been found in meteorites.[19]

The temperature minimum around 2.4 billion years goes along with a cosmic ray flux modulation by a variable star formation rate in the Milky Way. The reduced solar impact later results in a stronger impact of cosmic ray flux (CRF), which is hypothesized to lead to a relationship with climatological variations.

An alternative model of solar evolution may explain the faint young Sun paradox. In this model, the early Sun underwent an extended period of higher solar wind output. This caused a mass loss from the Sun on the order of 5−10 percent over its lifetime, resulting in a more consistent level of solar luminosity (as the early Sun had more mass, resulting in more energy output than was predicted). In order to explain the warm conditions in the Archean era, this mass loss must have occurred over an interval of about one billion years. However, records of ion implantation from meteorites and lunar samples show that the elevated rate of solar wind flux only lasted for a period of 0.1 billion years. Observations of the young Sun-like star π1 Ursae Majoris matches this rate of decline in the stellar wind output, suggesting that a higher mass loss rate can not by itself resolve the paradox.[20]

Examination of Archaean sediments appears inconsistent with the hypothesis of high greenhouse concentrations. Instead, the moderate temperature range may be explained by a lower surface albedo brought about by less continental area and the "lack of biologically induced cloud condensation nuclei". This would have led to increased absorption of solar energy, thereby compensating for the lower solar output.[21]

See also

References

  1. 1 2 Sagan, C.; Mullen, G. (1972). "Earth and Mars: Evolution of Atmospheres and Surface Temperatures". Science 177 (4043): 52–56. Bibcode:1972Sci...177...52S. doi:10.1126/science.177.4043.52. PMID 17756316.
  2. ↑ Gough, D. O. (1981). "Solar Interior Structure and Luminosity Variations". Solar Physics 74 (1): 21–34. Bibcode:1981SoPh...74...21G. doi:10.1007/BF00151270.
  3. ↑ Windley, B. (1984). The Evolving Continents. New York: Wiley Press. ISBN 0-471-90376-0.
  4. ↑ Schopf, J. (1983). Earth’s Earliest Biosphere: Its Origin and Evolution. Princeton, N.J.: Princeton University Press. ISBN 0-691-08323-1.
  5. ↑ Veizer, Jan (March 2005). "Celestial climate driver: a perspective from four billion years of the carbon cycle". Geoscience Canada 32 (1).
  6. ↑ Walker, James C. G. (June 1985). "Carbon dioxide on the early earth" (PDF). Origins of Life and Evolution of the Biosphere 16 (2): 117–127. Bibcode:1985OLEB...16..117W. doi:10.1007/BF01809466. Retrieved 2010-01-30.
  7. ↑ Pavlov, Alexander A.; Kasting, James F.; Brown, Lisa L.; Rages, Kathy A.; Freedman, Richard (May 2000). "Greenhouse warming by CH4 in the atmosphere of early Earth". Journal of Geophysical Research 105 (E5): 11981–11990. Bibcode:2000JGR...10511981P. doi:10.1029/1999JE001134.
  8. ↑ Ueno, Y.; Johnson, M. S.; Danielache, S. O.; Eskebjerg, C.; Pandey, A.; Yoshida, N. (August 2009). "Geological sulfur isotopes indicate elevated OCS in the Archean atmosphere, solving faint young sun paradox Ueno, Y.; Johnson, M. S.; Danielache, S. O.; Eskebjerg, C.; Pandey, A.; Yoshida, N.". Proceedings of the National Academy of Sciences 106 (35): 14784–14789. Bibcode:2009PNAS..10614784U. doi:10.1073/pnas.0903518106.
  9. ↑ Marty, B.; Zimmermann, L.; Pujol, M.; Burgess, R.; Philippot, P. (2013). "Nitrogen Isotopic Composition and Density of the Archean Atmosphere". Science 342 (6154): 101. arXiv:1405.6337. Bibcode:2013Sci...342..101M. doi:10.1126/science.1240971.
  10. ↑ "Climate puzzle over origins of life on Earth". Archived from the original on 4 October 2013. Retrieved 4 October 2013.
  11. ↑ Veizer, J. (1976). B. F. Windley, eds. The Early History of the Earth. London: John Wiley and Sons. p. 569. ISBN 0-471-01488-5.
  12. ↑ Zeebe, Richard (April 28, 2008). "Before fossil fuels, Earth’s minerals kept CO2 in check". University of Hawaiʻi at Mānoa. Retrieved 2010-01-30.
  13. ↑ Walker, J. C. G.; Hays, P. B.; Kasting, J. F. (October 20, 1981). "A negative feedback mechanism for the long-term stabilization of the earth's surface temperature" (PDF). Journal of Geophysical Research 86 (C10): 9776–9782. Bibcode:1981JGR....86.9776W. doi:10.1029/JC086iC10p09776. Retrieved 2010-01-30. Archived September 20, 2008, at the Wayback Machine.
  14. ↑ Hoffman, Paul F.; Kaufman, Alan J.; Halverson, Galen P.; Schrag, Daniel P. (August 28, 1998). "A Neoproterozoic Snowball Earth". Science 281 (5381): 1342–1346. Bibcode:1998Sci...281.1342H. doi:10.1126/science.281.5381.1342. PMID 9721097.
  15. ↑ Arevalo Jr, R., McDonough, W. F., & Luong, M. (2009). The K/U ratio of the silicate Earth: Insights into mantle composition, structure and thermal evolution. Earth and Planetary Science Letters, 278(3), 361–369
  16. ↑ http://curious.astro.cornell.edu/question.php?number=124
  17. ↑ Peale, S.J. Tidally induced volcanism. Celest. Mech. & Dyn. Astr. 87, 129–155, 2003.
  18. ↑ Shaviv, N. J. (2003). "Toward a solution to the early faint Sun paradox: A lower cosmic ray flux from a stronger solar wind". Journal of Geophysical Research 108 (A12): 1437. arXiv:astro-ph/0306477. Bibcode:2003JGRA..108.1437S. doi:10.1029/2003JA009997.
  19. ↑ Caffe, M. W.; Hohenberg, C. M.; Swindle, T. D.; Goswami, J. N. (February 1, 1987). "Evidence in meteorites for an active early sun". Astrophysical Journal Letters 313: L31–L35. Bibcode:1987ApJ...313L..31C. doi:10.1086/184826.
  20. ↑ Gaidos, Eric J.; Güdel, Manuel; Blake, Geoffrey A. (2000). "The faint young Sun paradox: An observational test of an alternative solar model". Geophysical Research Letters 27 (4): 501–504. Bibcode:2000GeoRL..27..501G. doi:10.1029/1999GL010740.
  21. ↑ Rosing, Minik T.; Bird, Dennis K.; Sleep, Norman H.; Bjerrum, Christian J. (April 1, 2010). "No climate paradox under the faint early Sun". Nature 464 (7289): 744–747. Bibcode:2010Natur.464..744R. doi:10.1038/nature08955. PMID 20360739.

Further reading

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