Estimates of heat flow in the deep mantle based on the power requirements for the geodynamo

By B. Buffett. 2002

185 citations recorded by the source corpus.

Subfields: Geophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/39049bf963ebc3e4dccc5d23d81b26e382585cf1

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Citations in the corpus

Thermal versus elastic heterogeneity in high‐resolution mantle circulation models with pyrolite composition: High plume excess temperatures in the lowermost mantle (2009, background): “…of the magnetic field, for which our current limited understanding provides estimates ranging from 0.1 to 3.5 TW [Roberts and Glatzmaier, 2000; Buffett, 2002; Roberts et al., 2003; Labrosse, 2003; Gubbins et al., 2003; Christensen and Tilgner, 2004], The total core heat loss may thus approach…”
Postperovskite phase transition and its geophysical implications (2006, background): “It corresponds to a global heat flux of 9– 13 TW across the CMB, which is sufficient to power the geodynamo in the outer core [Buffett, 2002].”
Reconciling dynamic and seismic models of Earth's lower mantle: The dominant role of thermal heterogeneity (2012, background): “…physics point towards a CMB temperature of 40007300K (e.g. Glatzmaier and Roberts, 1995; Kuang and Bloxham, 1997; Boehler, 2000; Alf e et al., 2002; Buffett, 2002; Gubbins et al., 2004; Nimmo et al., 2004; Hernlund et al., 2005; Nolet et al., 2006; Alf e et al., 2007; van der Hilst et al., 2007;…”
Energetics of the Core (2015, methodology): “…to be 5000 K. Roberts et al. (2003) used the results of the Glatzmaier and Roberts (1996) simulation to infer that 1-2 TW are required to power the dynamo, equivalent to an entropy production rate of 200-400 MW/K. Buffett (2002) suggested 0.1-0.5 TW and Buffett and Christensen (2007) 0.7-1 TW.”
Thermal and magnetic evolution of the Earth’s core (2003, methodology): “Using the dynamo model ofKuang and Bloxham (1997), Buffett (2002)proposed 0.1TW ≤ Φ ≤ 0.5TW, although without excluding the possibility of larger values.”
LINKS BETWEEN LONG‐LIVED HOT SPOTS, MANTLE PLUMES, D″, AND PLATE TECTONICS (2004, background): “One heuristic constraint is that core cooling is required to drive the geodynamo and produce the magnetic field observed at the surface of the Earth [e.g., Verhoogen, 1961; Gubbins, 1977; Stevenson, 1981; Loper, 1989; Buffett et al., 1996; Stevenson et al., 1983; Buffett, 2002; Stevenson, 2003].”
Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields (2006, background): “…related to inner core growth, are important because they put constraints on the age of the Earth’s inner core, the necessity for heat-producing elements such as40K in the core, and the degree to which convection in the Earth’s mantle is driven by heating from the core (Labrosse 2002; Buffett 2003).”
Dynamics and evolution of the deep mantle resulting from thermal, chemical, phase and melting effects (2012, background): “Buffett (2007) showed that if the pPv transition drives downwards flow then the heat flux can be much higher.”
Tomographic filtering of high‐resolution mantle circulation models: Can seismic heterogeneity be explained by temperature alone? (2009, result): “…seismology and mineral physics [e.g.,Glatzmaier and Roberts, 1995; Kuang and Bloxham, 1997; Boehler, 2000; Steinle-Neumann et al., 2001; Buffett, 2002;Gubbins et al., 2004;Nimmo et al., 2004;Nolet et al., 2006;Alfè et al., 2002, 2007; van derHilst et al., 2007; Steinberger and Holme,…”
Core–mantle boundary heat flow (2008, background): “1 TW when the structure of the predicted field is scaled to the spatial dimensions of the Earth's cor”
Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy (2006, background): “Global CMB heat flux on the order of a few terawatts is required to drive the geodynamo [Buffett, 2002].”
The influence of potassium on core and geodynamo evolution (2003, methodology): “In the absence of potassium, both entropy production and inner core growth rate have a nearly linear dependence on the core cooling rate dT c/dt (G1; G2), so the ratio of the two quantities is almost independent of dT c/dt (Fig. 4). This independence explains why it is difficult to obtain a small in”
Urey ratio and the structure and evolution of Earth's mantle (2008, background): “…order to take into account core-related observables, we have to face other sources of uncertainty such as the amount of ohmic dissipation required for the geodynamo [e.g., Buffett, 2002; Roberts et al., 2003] and the thermodynamic and chemical properties of the core [e.g., Davies, 2007].”