Promethei Terra is a large Martian region covering 3300 km at its broadest extent. It lies to the east of the massive Hellas basin. Like much of the southern part of the planet it is a heavily cratered, highland region. Promethei Terra was named for a classic albedo feature of Mars, with the original name derived from that of the Greek god Prometheus. Promethei Terra lies mostly in the Hellas quadrangle of Mars.
Lobate Debris Aprons
One very important feature common in Promethei Terra are piles of material surrounding cliffs. These materials are called lobate debris aprons (LDA's). Recently, research with the Shallow Radar on the Mars Reconnaissance Orbiter has provided strong evidence that the LDA's are glaciers that are covered with a thin layer of rocks. Large amounts of water ice are believed to be in the LDA's. Available evidence strongly suggests this area accumulated snow in the past. When the tilt (obliquity) of Mars increases the southern ice cap releases large amounts of water vapor. Climate models predict that when this occurs water vapor condenses and falls where LDAs are located. The tilt of the earth changes little because our relatively large moon keeps it stable. The two tiny Martian moons do not stabilize its planet, so the rotational axis of Mars undergoes large variations. It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as our moon stabilizes Earth; at times the tilt has even been greater than 80 degrees
Lobate debris aprons may be a major source of water for future Mars colonists. Their major advantage over other sources of Martian water are that they can easily mapped from orbit and they are closer to the equator where manned missions are more likely to land.
- Water on Mars
- Climate of Mars
- Glaciers on Mars
- Lobate Debris Apron
- Google Mars centered on Promethei Terra
- European Space Agency images of Promethei Terra
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- Holt, J. et al., 2008. Science 322:1235–1238.
- name= Touma J. and J. Wisdom. 1993. The Chaotic Obliquity of Mars. Science 259, 1294-1297.
- Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel. 2004. Long term evolution and chaotic diffusion of the insolation quantities of Mars. Icarus 170, 343-364.
- Geologic Map of Reull Vallis Region of Mars, includes the highlands of eastern Promethei Terra, by Astrogeology Science Center, U.S. Geological Survey
- Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention