Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars

  title={Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars},
  author={James W. Head and Gerhard Neukum and Ralf Jaumann and Harald Hiesinger and Ernst Hauber and Michael H. Carr and Ph. Masson and Bernard H. Foing and Harald Hoffmann and Mikhail A. Kreslavsky and Stephanie C. Werner and Sarah Milkovich and Stephan van Gasselt},
Images from the Mars Express HRSC (High-Resolution Stereo Camera) of debris aprons at the base of massifs in eastern Hellas reveal numerous concentrically ridged lobate and pitted features and related evidence of extremely ice-rich glacier-like viscous flow and sublimation. Together with new evidence for recent ice-rich rock glaciers at the base of the Olympus Mons scarp superposed on larger Late Amazonian debris-covered piedmont glaciers, we interpret these deposits as evidence for… 

An extended period of episodic northern mid-latitude glaciation on Mars during the Middle to Late Amazonian: Implications for long- term obliquity history

Mars is the only planet other than Earth in the Solar System that has a preserved nonpolar geological record of glaciation on its surface. Nonpolar ice deposits on Mars have been linked to variations

Wet-based glaciation on Mars

Mars is a glacial planet. It hosts water ice in large polar ice caps, and in thousands of ‘viscous flow features’ in its mid latitudes that are thought to be debris-covered water ice glaciers. These

Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin

Analysis of the insolation geometry of this pole-facing crater wall, and similar occurrences in other craters at these latitudes on Mars, shows that they are uniquely favored for accumulation of snow and ice, and a relatively more rapid exposure to warmer summer temperatures.

Extensive valley glacier deposits in the northern mid-latitudes of Mars : Evidence for Late Amazonian obliquitydriven obliquitydriven obliquitydriven climate change

Understanding spin orbital parameter-driven climate change on Mars prior to ~ 20 Ma ago requires geological evidence because numerical solutions for that period are chaotic and non-unique. We show



Tropical Mountain Glaciers on Mars: Evidence for Amazonian Climate Change

Introduction and background: Polar deposits on Mars represent one of the most significant current volatile reservoirs on the planet and these, together with high-latitude surface and near-surface

Recent and episodic volcanic and glacial activity on Mars revealed by the High Resolution Stereo Camera

It is shown that calderas on five major volcanoes on Mars have undergone repeated activation and resurfacing during the last 20 per cent of martian history, with phases of activity as young as two million years, suggesting that the volcanoes are potentially still active today.

Ice flow and rock glaciers on Mars

Several geologic features suggest the presence of rock glaciers on the surface of Mars. These features include lobate debris aprons, concentric crater fill and lineated valley fill. The lateral

Recent ice ages on Mars

Evidence is shown that dusty, water-ice-rich mantling deposits on Mars formed during a geologically recent ice age that occurred from about 2.1 to 0.4 Myr ago, a key pacemaker of ice ages on the Earth.

Cold-based Mountain Glaciers on Mars: Western Arsia Mons Fan-shaped Deposits

Surface environmental conditions on Mars are currently extremely cold and hyperarid, most equivalent to polar deserts on Earth. Coupling newly acquired Mars data with fieldbased observations

Discovery of a flank caldera and very young glacial activity at Hecates Tholus, Mars

New image and topographic data from the High Resolution Stereo Camera reveal previously unknown traces of an explosive eruption on the northwestern flank of the shield volcano Hecates Tholus, meaning that large-scale explosive volcanism on Mars was not confined to the planet's early evolution.

Ancient glaciation on Mars

A large number of anomalous landforms on Mars can be attributed to glaciation, including the action of ice and meltwater. Glacial landscapes are concentrated south of lat -33° and in the Northern

Formation of patterned ground and sublimation till over Miocene glacier ice in Beacon Valley, southern Victoria Land, Antarctica

A thin glacial diamicton, informally termed Granite drift, occupies the floor of central Beacon Valley in southern Victoria Land, Antarctica. This drift is 40 Ar/ 39 Ar analyses of presumed in situ