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Evolution of Staircase Structures in Diffusive Convection
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Can mantle convection be self-regulated?

Jun Korenaga1

  • 1Department of Geology and Geophysics, Yale University, P.O. Box 208109, New Haven, CT 06520-8109, USA.

Science Advances
|August 24, 2016
PubMed
Summary

Planetary mantle convection likely does not self-regulate heat loss. Accounting for melting effects on viscosity prevents sufficient thermal adjustment, making planetary evolution sensitive to formation history and chance.

Area of Science:

  • Solid Earth Sciences
  • Planetary Science
  • Geophysics

Background:

  • The concept of self-regulating mantle convection, where surface heat loss adjusts to internal heat production, has been influential for decades.
  • This idea, first proposed by Urey, intuitively suggests a stable thermal state for terrestrial planets.
  • However, achieving self-regulation depends critically on the relationship between thermal adjustment rates and mantle temperature.

Purpose of the Study:

  • To investigate whether self-regulating mantle convection is physically plausible.
  • To determine the influence of mantle melting on viscosity and its effect on thermal regulation.
  • To assess the implications for the thermal evolution and formation sensitivity of terrestrial planets.

Main Methods:

  • The study likely involves numerical modeling or theoretical analysis of mantle convection.
Keywords:
Heat flowplanetary evolutionthermal budget

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  • It incorporates the effect of mantle melting on the rheological properties (viscosity) of the mantle.
  • The research examines the thermal adjustment rate in relation to mantle temperature and convection dynamics.

    • Main Results:

    • The analysis demonstrates that the thermal adjustment rate is insufficient for self-regulation when mantle melting effects on viscosity are considered.
    • This holds true irrespective of the specific style or regime of mantle convection.
    • Planetary evolution appears to be significantly influenced by factors beyond simple thermal equilibrium.

    Conclusions:

    • Terrestrial planet evolution is likely not in a state of thermal equilibrium.
    • Planetary formation histories and their inherent "chance factors" play a crucial role in determining a planet's evolutionary path.
    • More massive planets than Earth may be even more susceptible to the impact of initial formation conditions.