Ancient Geodynamics and Global-Scale Hydrology on Mars

  title={Ancient Geodynamics and Global-Scale Hydrology on Mars},
  author={Roger J. Phillips and Maria T. Zuber and Sean C. Solomon and Matthew P. Golombek and Bruce M. Jakosky and William Bruce Banerdt and David E. Smith and Rebecca M. E. Williams and Brian M. Hynek and Oded Aharonson and Steven Hauck II},
  pages={2587 - 2591}
Loading of the lithosphere of Mars by the Tharsis rise explains much of the global shape and long-wavelength gravity field of the planet, including a ring of negative gravity anomalies and a topographic trough around Tharsis, as well as gravity anomaly and topographic highs centered in Arabia Terra and extending northward toward Utopia. The Tharsis-induced trough and antipodal high were largely in place by the end of the Noachian Epoch and exerted control on the location and orientation of… 

Topographic Change of the Dichotomy Boundary Suggested by Crustal Inversion

Linear negative gravity anomalies in Acidalia Planitia along the eastern edge of Tempe Terra and along the northern edge of Arabia Terra have been noted in Mars Global Surveyor gravity fields. Once


Anomalous aspects of Martian geology are explained by a theory that incorporates the onset and termination of a core dynamo, associated with an early regime of plate tectonics during the first few

Geophysical evidence supports migration of Tharsis volcanism on Mars

Tharsis swell represents the largest area of volcanism on Mars and sits adjacent to the dichotomy between the northern lowlands and southern highlands. While a number of investigators have proposed


  • J. Dohm
  • Environmental Science, Geology
  • 2002
Introduction. Throughout the recorded history of Mars, liquid water has shaped its landscape into a number of distinct morphologic types, including prominent features such as the circum-Chryse and

Hemispheres Apart: The Crustal Dichotomy on Mars

The hemispheric dichotomy is a fundamental feature of Mars, expressed by a physiographic and geologic divide between the heavily cratered southern highlands and the relatively smooth plains of the

Late Tharsis formation and implications for early Mars

The rotational figure of Mars (that is, its equilibrium shape) and its surface topography before Tharsis formed, when the spin axis of the planet was controlled by the difference in elevation between the northern and southern hemispheres (hemispheric dichotomy), is calculated.

Variations in Martian Lithospheric Strength Based on Gravity/Topography Analysis

We applied localized gravity/topography admittance and correlation analysis, as well as the Markov chain Monte Carlo method, to invert for loading and flexural parameters of 21 subregions on Mars



Evolution of the Tharsis Province of Mars: The importance of heterogeneous lithospheric thickness and volcanic construction

The Tharsis province of Mars is a broad region characterized by anomalously elevated topography, a positive free-air gravity anomaly, and extensive volcanic and tectonic activity. The evolution of

The role of lithospheric stress in the support of the Tharsis Rise

The Tharsis rise on Mars is a broad topographic high covered by volcanic plains and capped by large volcanoes. The geoid high associated with Tharsis shows that shallow isostatic compensation is not

Lithospheric-scale buckling and thrust structures on Mars: The Coprates rise and south Tharsis ridge belt

Detailed photogeologic mapping documents for the first time the deformation sequence of the Coprates rise. Materials of Middle Noachian through perhaps Early Hesperian age were involved in the

Voluminous volcanism on early Mars revealed in Valles Marineris

The relative rates and importance of impact cratering, volcanism, erosion, and the deposition of sediments to the early geological history of Mars are poorly known. That history is recorded in the

Geomorphic evolution of the Martian highlands through ancient fluvial processes

Craters in the Martian highlands are preserved in various stages of degradation. As a result of an erosional process active from the Middle Noachian (4.40–3.92 b.y.) through the Hesperian (3.55–1.8

Mars without Tharsis

The significant power in the Martian gravitational field due to the Tharsis rise may mask or modify gravitational signatures that contain important information on Martian geophysical processes. In

The Martian drainage system and the origin of valley networks and fretted channels

Outflow channels provide strong evidence for abundant water near the Martian surface and an extensive groundwater system. Collapse of the surface into some channels suggests massive subsurface

Support of long‐wavelength loads on Venus and implications for internal structure

A thin-shell formulation for computing stress distributions on the surfaces of one-plate planets is developed. The lithospheric model includes laterally varying density anomalies at two depths,

Cratering and obliteration history of Mars

The review presented is based mainly on the pre-Viking literature. Early interpretations of the Mariner 4 pictures of Martian craters are considered along with interpretations of Mariner 9 pictures.

Volatile budget of Kilauea volcano

The volatile content of magma in the reservoirs of active volcanoes has an important bearing on problems of petrogenesis, magma degassing, eruption mechanisms, eruption forecasting and monitoring and