Where is Mars' Ice? Constraints from impact craters and lobate debris aprons on a mid-latitude reservoir

 Ancient features such as outflow channels and phyllosilicate mineral outcrops, suggest a large amount of water was once present on the Martian surface. The volume of water required to form these features exceeds the current inventory of water frozen at the Martian poles. Observations of surface craters and large flow features known as lobate debris aprons provide insight into the amount of water ice stored in mid-latitudes.


Mars: The water story and prospects for life

Recent missions to Mars have provided new evidence that early Mars was at least episodically earth-like with rivers, lakes and possibly oceans, and high rates of aqueous weathering and erosion. Life appears to have arisen early on Earth. Did some form of life start on Mars when conditions on the two planets were similar? Conditions on Mars subsequently changed to become much less hospitable but life, if started, may have maintained a tenuous foothold in isolated niches.

Atmospheric Escape and Aurora on Mars

Measurements of magnetic fields and charged particles near Mars made over the past 4 decades teach us about its plasma environment, upper atmosphere, near-surface environment, subsurface, and deep interior. The upper atmosphere and plasma environment of Mars are of interest because they are the sites of energy exchange between the planet and its surroundings, dominated by the Sun and solar wind. It is difficult to understand the state and evolution of the Martian system without understanding this important upper boundary.

The Surface of Mars: Mineralogy as an Indicator of Water and Environmental Conditions

The surface mineralogy of Mars provides clues to its geologic history, including aqueous processes. Phyllosilicates and sulfates are key indicators of water on Mars and appear to have occurred in the Noachian and Hesperian, respectively. Dr. Bishop will discuss what we know about Martian mineralogy from orbital and landed missions, meteorites, and terrestrial analog studies.

Death of the Martian Dynamo

Unlike Earth, Mars has no global dynamo-driven magnetic field. However, strongly magnetized crust tells us that such a field existed in the past. The reasons for, and timing and manner of, its demise is an important question in Mars science, with ramifications for the evolution of the atmosphere and the stability of liquid water on the Martian surface. Dr.

Geological record of recent climate change on Mars

Climate on Mars changes at a wide range of time scales; these changes leave observable traces in the geological record of the planet. Recent decade of intensive orbital imaging of Mars has revealed a fascinating set of geologically young features indicating different climate conditions: recent gullies, surprisingly dynamic high-latitude landscapes, a wealth of new information about the polar layered deposits, traces of huge extinct tropical mountain glaciers, impressive remnants of wide-spread mid-latitude glaciation, etc.

True Polar Wander and Climate on Late Hesperian/Amazonian Mars

True Polar Wander (TPW) can be a major driver of tectonics and climate change on one-plate planets, such as post-Noachian Mars. But did TPW actually occur? I will summarize work at Berkeley testing this hypothesis, and its place in understanding the last three billion years of climate change on Mars. I will also present results from an ongoing Berkeley/Ames collaboration using General Climate Models to further test late-stage polar wander. This talk may not turn your view of Mars upside down, but it could rotate it by about 8 degrees. 

Experimental determination of the effect of salts, regolith, and wind on the stability of water under Martian conditions

Many fundamental processes on Mars require an understanding of the temperature and pressure conditions at the Martian surface. In particular, the stability of liquid water is a key factor in formation of gully features, and is significant to the possibly for life on Mars. Dr. Chittenden will discuss her experimental work on the stability of water under martian conditions, performed at the University of Arkansas in the Mars planetary simulation chamber. Her results suggests concentrated brine water may remain liquid on the Martian surface longer than previously thought.

Google Earth, now with Mars!

Google, Inc., has released Google Earth 5.0 which contains a Mars 3D mode. Working with engineers at Google, we helped collect, parse, and organize the vast store of Mars geospatial data available to the public into a form that could be used by Google Earth. The Mars mode presents data acquired both from orbit and on the surface, presented fully integrated into the Google Earth geospatial browser.

Surface modifications by winds on Earth, Mars, Venus, and Titan

Windblown dunes, ripples, and erosional features are seen on Earth, Venus, and Titan, while on Mars these features are ubiquitous and reflect the dominant agent of surface modification. Although the fundamental process is similar, the environments on these planetary objects are substantially different. Simulations conducted in the Planetary Aeolian Laboratory at NASA-Ames, coupled with field work and modeling, enable analyses of wind-related features and processes on planetary surfaces.


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