Mantle convection

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Earth cross-section showing location of upper (3) and lower (5) mantle
Calculated Earth's temperature vs. depth. Dashed curve: Layered mantle convection; Solid curve: Whole mantle convection.[1]
Whole mantle convection
A superplume generated by cooling processes in the mantle.[2]

Mantle convection is the slow creeping motion of Earth's solid silicate mantle caused by convection currents carrying heat from the interior of the Earth to the surface.[3][4] The Earth's surface lithosphere, which rides atop the asthenosphere (the two components of the upper mantle), is divided into a number of plates that are continuously being created and consumed at their opposite plate boundaries. Accretion occurs as mantle is added to the growing edges of a plate, associated with seafloor spreading. This hot added material cools down by conduction and convection of heat. At the consumption edges of the plate, the material has thermally contracted to become dense, and it sinks under its own weight in the process of subduction usually at an ocean trench.[5]

This subducted material sinks through the Earth's interior. Some subducted material appears to reach the lower mantle,[6] while in other regions, this material is impeded from sinking further, possibly due to a phase transition from spinel to silicate perovskite and magnesiowustite, an endothermic reaction.[7]

The subducted oceanic crust triggers volcanism, although the basic mechanisms are varied. Volcanism may occur due to processes that add buoyancy to partially melted mantle causing an upward flow due to a decrease in density of the partial melt.

Secondary forms of convection that may result in surface volcanism are postulated to occur as a consequence of intraplate extension[8] and mantle plumes.[1]

It is because the mantle can convect that the tectonic plates are able to move around the Earth's surface.[9]

Mantle convection seems to have been much more active during the Hadean period, resulting in gravitational sorting of heavier molten iron, and nickel elements and sulphides in the core, and lighter silicate minerals in the mantle.

Types of convection[edit]

During the late 20th century, there was significant debate within the geophysics community as to whether convection is likely to be 'layered' or 'whole'. See for example, Donald Lawson Turcotte; Gerald Schubert (2002). Geodynamics (2nd ed.). Cambridge University Press. ISBN 0-521-66624-4. ; and also: Gerald Schubert; Donald Lawson Turcotte; Peter Olson (2001). Cited work. p. 616. ISBN 0-521-79836-1. . Although elements of this debate still continue, results from seismic tomography, numerical simulations of mantle convection and examination of Earth's gravitational field are all beginning to suggest the existence of 'whole' mantle convection, at least at the present time. In this model, cold, subducting oceanic lithosphere descends all the way from the surface to the core-mantle boundary (CMB) and hot plumes rise from the CMB all the way to the surface.[10] This picture is strongly based on the results of global seismic tomography models, which typically show slab and plume-like anomalies crossing the mantle transition zone.

Although it is now well accepted that subducting slabs cross the mantle transition zone and descend into the lower mantle, debate about the existence and continuity of plumes persists, with important implications for the style of mantle convection. This debate is linked to the controversy regarding whether intraplate volcanism is caused by shallow, upper-mantle processes or by plumes from the lower mantle.[8] Many geochemistry studies have argued that the lavas erupted in intraplate areas are different in composition from shallow-derived mid ocean ridge basalts (MORB). Specifically, they typically have elevated Helium-3 - Helium-4 ratios. Being a primordial nuclide, Helium-3 is not naturally produced on earth. It also quickly escapes from earth's atmosphere when erupted. The elevated He-3/He-4 ratio of Ocean Island Basalts (OIBs) suggest that they must be sources from a part of the earth that has not previously been melted and reprocessed in the same way as MORB source has been. This has been interpreted as their originating from a different, less well-mixed, region, suggested to be the lower mantle. Others, however, have pointed out that geochemical differences could indicate the inclusion of a small component of near-surface material from the lithosphere.

Speed of convection[edit]

Typical mantle convection speed is 20 mm/yr near the crust but can vary quite a bit.[11][12][13] The small scale convection in the upper mantle is much faster than the convection near the core. (See whole-mantle discussion above.) A single shallow convection cycle takes on the order of 50 million years, though deeper convection can be closer to 200 million years.[14]

Creep in the Mantle[edit]

Since the mantle is primarily composed of olivine ((Mg,Fe)2SiO4), the rheological characteristics of the mantle are largely those of olivine. Additionally, due to the varying temperatures and pressures between the lower and upper mantle, a variety of creep processes can occur with dislocation creep dominating in the lower mantle and diffusional creep occasionally dominating in the upper mantle. However, there is a large transition region in creep processes between the upper and lower mantle and even within each section, creep properties can change strongly with location and thus temperature and pressure. In the power law creep regions, the creep equation fitted to data with n = 3-4 is standard.[15]

The strength of olivine not only scales with its melting temperature, but also is very sensitive to water and silica content. The solidus depression by impurities, primarily Ca, Al, and Na, and pressure affects creep behavior and thus contributes to the change in creep mechanisms with location. While creep behavior is generally plotted as homologous temperature versus stress, in the case of the mantle it is often more useful to look at the pressure dependence of stress. Though stress is simple force over area, defining the area is difficult in geology. Equation 1 demonstrates the pressure dependence of stress. Since it is very difficult to simulate the high pressures in the mantle (1MPa at 300–400 km), the low pressure laboratory data is usually extrapolated to high pressures by applying creep concepts from metallurgy.[16]

(1) [16]

Most of the mantle has homologous temperatures of 0.65-0.75 and experiences strain rates of 10^-14 – 10^-16 1/s. Stresses in mantle are dependent on density, gravity, thermal expansion coefficients, temperature differences driving convection, and distance convection occurs over, all of which give stresses around a fraction of 3-30MPa. Due to the large grain sizes (at low stresses as high as several mm), it is unlikely that Nabarro-Herring (NH) creep truly dominates. Given the large grain sizes, dislocation creep tends to dominate. 14 MPa is the stress below which diffusional creep dominates and above which power law creep dominates at 0.5Tm of olivine. Thus, even for relatively low temperatures, the stress diffusional creep would operate at is too low for realistic conditions. Though the power law creep rate increases with increasing water content due to weakening, reducing activation energy of diffusion and thus increasing the NH creep rate, NH is generally still not large enough to dominate. Nevertheless, diffusional creep can dominate in very cold or deep parts of the upper mantle. Additional deformation in the mantle can be attributed to transformation enhanced ductility. Below 400 km, the olivine undergoes a pressure induced phase transformation into spinel and can cause more deformation due to the increased ductility.[16] Further evidence for the dominance of power law creep comes from preferred lattice orientations as a result of deformation. Under dislocation creep, crystal structures reorient into lower stress orientations. This does not happen under diffusional creep, thus observation of preferred orientations in samples lends credence to the dominance of dislocation creep.[17]

See also[edit]

References[edit]

  1. ^ a b Kent C. Condie (1997). Plate tectonics and crustal evolution (4th ed.). Butterworth-Heinemann. p. 5. ISBN 0-7506-3386-7. 
  2. ^ Ctirad Matyska & David A Yuen (2007). "Figure 17 in Lower-mantle material properties and convection models of multiscale plumes". Plates, plumes, and planetary processes. Geological Society of America. p. 159. ISBN 0-8137-2430-9. 
  3. ^ Kobes, Randy and Kunstatter, Gabor."Mantle Convection". Physics Department, University of Winnipeg. Retrieved 3 January 2010.
  4. ^ Ricard, Y. (2009). "2. Physics of Mantle Convection". In David Bercovici and Gerald Schubert. Treatise on Geophysics: Mantle Dynamics. 7. Elsevier Science. 
  5. ^ Gerald Schubert; Donald Lawson Turcotte; Peter Olson (2001). "Chapter 2: Plate tectonics". Mantle convection in the earth and planets. Cambridge University Press. p. 16 ff. ISBN 0-521-79836-1. 
  6. ^ Fukao, Yoshio; Obayashi, Masayuki; Nakakuki, Tomoeki; Group, the Deep Slab Project (2009-01-01). "Stagnant Slab: A Review". Annual Review of Earth and Planetary Sciences. 37 (1): 19–46. doi:10.1146/annurev.earth.36.031207.124224. 
  7. ^ Gerald Schubert; Donald Lawson Turcotte; Peter Olson. "§2.5.3: Fate of descending slabs". Cited work. p. 35 ff. ISBN 0-521-79836-1. 
  8. ^ a b Foulger, G.R. (2010). Plates vs. Plumes: A Geological Controversy. Wiley-Blackwell. ISBN 978-1-4051-6148-0. 
  9. ^ Moresi, Louis; Solomatov, Viatcheslav (1998). "Mantle convection with a brittle lithosphere: thoughts on the global tectonic styles of the Earth and Venus". Geophysical Journal International. 133: 669–682. Bibcode:1998GeoJI.133..669M. doi:10.1046/j.1365-246X.1998.00521.x. CiteSeerX: 10.1.1.30.5989. 
  10. ^ Montelli, R; Nolet, G; Dahlen, FA; Masters, G; Engdahl ER; Hung SH (2004). "Finite-frequency tomography reveals a variety of plumes in the mantle". Science. 303 (5656): 338–43. Bibcode:2004Sci...303..338M. doi:10.1126/science.1092485. PMID 14657505. 
  11. ^ Small-scale convection in the upper mantle beneaththe Chinese Tian Shan Mountains, http://www.vlab.msi.umn.edu/reports/allpublications/files/2007-pap79.pdf
  12. ^ Polar Wandering and Mantle Convection, http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?bibcode=1972IAUS...48..212T&db_key=AST&page_ind=0&data_type=GIF&type=SCREEN_VIEW&classic=YES
  13. ^ Picture showing convection with velocities indicated. http://www.iris.edu/hq/gallery/photo/4344
  14. ^ Thermal Convection with a Freely Moving Top Boundary, See section IV Discussion and Conclusions http://physics.nyu.edu/jz11/publications/ConvecA.pdf
  15. ^ Weertman, J.; White, S.; Cook, Alan H. (1978-02-14). "Creep Laws for the Mantle of the Earth [and Discussion]". Philosophical Transactions of the Royal Society of London A: Mathematical, Physical and Engineering Sciences. 288 (1350): 9–26. doi:10.1098/rsta.1978.0003. ISSN 1364-503X. 
  16. ^ a b c Borch, Robert S.; Green, Harry W. (1987-11-26). "Dependence of creep in olivine on homologous temperature and its implications for flow in the mantle". Nature. 330 (6146): 345–348. Bibcode:1987Natur.330..345B. doi:10.1038/330345a0. 
  17. ^ Karato, Shun-ichiro; Wu, Patrick (1993-05-07). "Rheology of the Upper Mantle: A Synthesis". Science. 260 (5109): 771–778. Bibcode:1993Sci...260..771K. doi:10.1126/science.260.5109.771. ISSN 0036-8075. PMID 17746109.