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Mars's Tharsis volcanic region may not have influenced early valley networks. New models suggest topography before Tharsis formation explains valley orientations and water distribution on early Mars.

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Area of Science:

  • Planetary Science
  • Geology
  • Climate Science

Background:

  • The Tharsis region on Mars, the solar system's largest volcanic complex, grew over billions of years.
  • Its immense mass is thought to have caused true polar wander (TPW), reorienting Mars and positioning Tharsis near the equator.
  • Previous theories proposed Tharsis influenced the orientation of early Martian valley networks.

Purpose of the Study:

  • To investigate the influence of the Tharsis volcanic load on the orientation of early Martian valley networks.
  • To reconstruct Mars's topography and rotational figure before the Tharsis region formed.
  • To test whether pre-Tharsis topography can explain observed valley network patterns.

Main Methods:

  • Calculated the rotational figure (equilibrium shape) of Mars prior to Tharsis formation.
  • Reconstructed the planet's surface topography in a pre-Tharsis, pre-TPW state.
  • Analyzed topographic gradients and compared them with observed valley network orientations.

Main Results:

  • Observed valley network directions are consistent with topographic gradients on Mars before the Tharsis load existed.
  • Valley distribution aligns with a southern hemisphere latitudinal band in the pre-TPW frame.
  • Climate models predict preferential ice/water accumulation in this band based on pre-TPW topography.

Conclusions:

  • The Tharsis load is not required to explain the orientation of early Martian valley networks.
  • A late growth phase for Tharsis, concurrent with valley incision, has significant implications for early Martian geology and climate.
  • This revised timeline suggests potential glacial environments and links volcanic outgassing to surface water stability.