Origin of mountains on Io by thrust faulting and large-scale mass movements

  title={Origin of mountains on Io by thrust faulting and large-scale mass movements},
  author={Schenk and Bulmer},
  volume={279 5356},
Voyager stereoimages of Euboea Montes, Io, indicate that this mountain formed when a large crustal block was uplifted 10.5 kilometers and tilted by approximately 6 degrees. Uplift triggered a massive slope failure on the northwest flank, forming one of the largest debris aprons in the solar system. This slope failure probably involved relatively unconsolidated layers totaling approximately 2 kilometers in thickness, overlying a rigid crust (or lithosphere) at least 11 kilometers thick. Mountain… 

Mountain building on Io driven by deep faulting

The high relief on Jupiter’s moon Io has been linked to compression due to global subsidence. Simulations show that Io’s mountains may form along thrust faults that initiate at the lithosphere’s base

Big Mountain, Big Landslide on Jupiter's Moon, Io

Clear evidence of what this internal heat is doing to Io's surface was first revealed in the 1979 Voyager spacecraft images. Spectacular scenes of active volcanic eruption plumes, a surface lacking

Mountains on Io: High‐resolution Galileo observations, initial interpretations, and formation models

During three close flybys in late 1999 and early 2000 the Galileo spacecraft acquired new observations of the mountains that tower above Io's surface. These images have revealed surprising variety in

Chaos on Io: A model for formation of mountain blocks by crustal heating, melting, and tilting

Mountains are distributed across the surface of Io, the fiercely tidally heated moon of Jupiter. The large crustal thicknesses implied by their great heights can be reconciled with Io's high heat

The mountains of Io: Global and geological perspectives from Voyager and Galileo

To search for local and global scale geologic associations that may be related to the internal dynamics of lo, we have completed a global catalog of all mountains and volcanic centers. We have

Evidence of thrust faulting and widespread contraction of Ceres

The surface of the dwarf planet Ceres is considered to be dominated by geological processes typical of small bodies or medium-sized icy bodies, such as impact cratering1,2; there are also features of

Select problems in planetary structural Geology: Global-scale tectonics on Io, regional-scale kinematics on Venus, and local-scale field analyses on Earth with application to Mars

Io's mountains are cataloged in order to investigate their formation. Of the 101 mountains imaged with sufficient coverage and resolution for further analysis, 4 are volcanoes, and 97 are tectonic



Further evidence for a mass movement origin of the Olympus Mons aureole

Analysis of the ridge, graben, and fracture patterns on the aureole material surrounding Olympus Mons lends further support to an origin by gravity sliding of the outer flanks of the shield. The

Structure of the Laramide Wind River Uplift, Wyoming, from Cocorp deep reflection data and from gravity data

The question of the structure of the Wind River uplift, a Laramide foreland structure in Wyoming, has been answered by Consortium for Continental Reflection Profiling (Cocorp) deep crustal reflection

Geology and topography of Ra Patera, Io, in the Voyager era: Prelude to eruption

Voyager era stereo images are used to map the geology and topography of Ra Patera (a major active volcanic center and possible site of sulfur eruptions on Io). The summit of Ra Patera reaches only ∼1

A large landslide on Mars

A large landslide deposit on the south wall of Gangis Chasma contains at least 100 billion m 3 of material that moved 60 km across the trough floor at a speed of more than 100 km/hr. The deposit

Mass Wasting and Ground Collapse in Terrains of Volatile-Rich Deposits as a Solar System-Wide Geological Process: The Pre-Galileo View

The polar terrains of Mars are covered in many places with irregular pits and retreating scarps, as are some of the surfaces of the outer-planet satellites. These features are interpreted by us as

The Olympus Mons Aureole: Formation by gravitational spreading

New observations of the aureole deposits of Olympus Mons are in agreement with previous suggestions that the aureole lobes could have been formed by movement under gravity away from the observed

Hot spots on Io: Initial results from Galileo's near infrared mapping spectrometer

The Near‐Infrared Mapping Spectrometer on Galileo has monitored the volcanic activity on Io since June 28, 1996. This paper presents preliminary analysis of NIMS thermal data for the first four

Io's heat flow from infrared radiometry: 1983–1993

We report the following results from a decade of infrared radiometry of Io: (1) The average global heat flow is more than ∼2.5 W m−2, (2) large warm (≤200 K) volcanic regions dominate the global heat

Time-Variable Phenomena in the Jovian System

The current state of knowledge of dynamic processes in the Jovian system is assessed and summaries are provided of both theoretical and observational foundations upon which future research might be

Erosional scarps on Io

Irregular or fretted scarps on Io are similar to those found on Earth and Mars. A sapping mechanism involving liquid SO2 is proposed to explain these complexly eroded terrains on Io.