Terrestrial planet evolution in the stagnant-lid regime: Size effects and the formation of self-destabilizing crust

  title={Terrestrial planet evolution in the stagnant-lid regime: Size effects and the formation of self-destabilizing crust},
  author={Joseph Ghilarducci O'Rourke and Jun Korenaga},

Thermal evolution of Venus with argon degassing

The Physics of Changing Tectonic Regimes: Implications for the Temporal Evolution of Mantle Convection and the Thermal History of Venus

Given similar sizes and compositions, Venus invites comparisons with Earth. While Earth convects in the plate tectonic regime, Venus' current and past tectonic states remain uncertain. Venus' impact

The habitability of a stagnant-lid Earth

Context. Plate tectonics is considered a fundamental component for the habitability of the Earth. Yet whether it is a recurrent feature of terrestrial bodies orbiting other stars or unique to the

The Southern polar giant impact hypothesis for the origin of the Martian dichotomy and the evolution of volcanism on mars

We demonstrate via numerical simulations that the impact of a ~ lunar-sized body with Mars is capable of creating a hemispherical magma ocean that upon cooling and solidification resulted in the

Carbon cycling and interior evolution of water-covered plate tectonics and stagnant-lid planets

Aims. The long-term carbon cycle for planets with a surface entirely covered by oceans works differently from that of the present-day Earth because inefficient erosion leads to a strong dependence of

Diffusion of volatiles in hot stagnant-lid regime planets

  • G. Bromiley
  • Geology, Physics
    Planetary and Space Science
  • 2020

Can mantle convection be self-regulated?

It is shown that, if the effect of mantle melting on viscosity is taken into account, the adjustment rate cannot be sufficiently high to achieve self-regulation, regardless of the style of mantle convection.

A mushy Earth's mantle for more than 500 Myr after the magma ocean solidification

In its early evolution, the Earth mantle likely experienced several episodes of complete melting enhanced by giant impact heating, short-lived radionuclides heating and viscous dissipation during



Scaling of time‐dependent stagnant lid convection: Application to small‐scale convection on Earth and other terrestrial planets

Small-scale convection associated with instabilities at the bottom of the lithospheric plates on the Earth and other terrestrial planets occurs in the stagnant lid regime of temperature-dependent

Scaling of stagnant-lid convection with Arrhenius rheology and the effects of mantle melting

SUMMARY On the basis of numerical modelling and scaling analysis, a few modifications are proposed for the scaling of stagnant-lid convection, in order to make it more applicable to the thermal


We study the thermal evolution of super-Earths with a one-dimensional (1D) parameterized convection model that has been adopted to account for a strong pressure dependence of the viscosity. A

The influence of mantle melting on the evolution of Mars

Geological consequences of super‐sized Earths

The discovery of terrestrial‐scale extrasolar planets, and their calculated abundance in the galaxy, has prompted speculation on their surface conditions and thermal structure. Both are dependent on

Thermal and crustal evolution of Mars

[1] We present a coupled thermal-magmatic model for the evolution of Mars' mantle and crust that may be consistent with estimates of the average crustal thickness and crustal growth rate. By coupling


We provide estimates of volcanism versus time for planets with Earth-like composition and masses 0.25–25 M⊕, as a step toward predicting atmospheric mass on extrasolar rocky planets. Volcanism

Modeling the Volcanism on Mars

The total amount of melt produced in Mars during its evolution is estimated by means of a parameterized, one-dimensional, analytic mantle convection model that assumes a stagnant lid and whole

Non-Newtonian Stagnant Lid Convection and Magmatic Resur facing on Venus☆

Abstract Mantle convection on Venus is likely to occur in the regime known as stagnant lid convection. We investigate this regime for internally heated convection with temperature- and