Tidal heating and convection in Io

@article{Moore2003TidalHA,
  title={Tidal heating and convection in Io},
  author={William B. Moore},
  journal={Journal of Geophysical Research},
  year={2003},
  volume={108},
  pages={5096}
}
  • W. Moore
  • Published 1 August 2003
  • Physics
  • Journal of Geophysical Research
[1] The prodigious heat flux emitted from the surface of Jupiter's moon Io is produced in the interior of the satellite by viscoelastic dissipation of tidal energy and is generally thought to be brought to the surface by convective motions. New models of Io's equilibrium thermal state are constructed using self-consistent calculations of tidal heating and convective heat transport. These models show that while a high-temperature convective equilibrium exists, it falls an order of magnitude… 

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References

SHOWING 1-10 OF 20 REFERENCES

The Thermal State of Io

Abstract A novel heat balance is proposed for Io's mantle in which heat produced by tidal dissipation is brought to the surface by rapid ascent of magma, rather than by convection. This is

Heat transfer and convection currents

  • D. Tozer
  • Physics
    Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences
  • 1965
‘Es gibt nichts praktischeres als die Theorie ’ (ludwig boltzmann—Vorlesungen 1895) The possible causes of convection in the Earth’s mantle are examined, and it is concluded that radiogenic heating

A self sustained magnetic field on Io

Stagnant lid convection in a spherical shell

Thermal-orbital histories of viscoelastic models of Io (J1)

Heat transport efficiency for stagnant lid convection with dislocation viscosity: Application to Mars and Venus

Mantle convection on Mars and Venus is likely to occur in the regime known as stagnant lid convection. We perform thermal boundary layer analyses as well as finite element simulations of stagnant lid

Io's thermal emission from the Galileo photopolarimeter-radiometer.

Mapping of Loki in I24 shows uniform temperatures for most of Loki Patera and high temperatures in the southwest corner, probably resulting from an eruption that began 1 month before the observation.

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