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While Mars's climate has similarities to Earth's, including periodic ice ages, there are also important differences, such as much lower thermal inertia. Mars' atmosphere has a scale height of approximately 11 km (36,000 ft), 60% greater than that on Earth. The climate is of considerable relevance to the question of whether life is or ever has ...
Mars climate simulation models date as far back as the Viking missions to Mars. Most Mars climate simulation models were written by individual researchers that were never reused or open-sourced. By the 1990s the need for a unified model codebase came into being, due to the general impact of the internet on climate modelling and research. This ...
The Mare Australe quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Mare Australe quadrangle is also referred to as MC-30 (Mars Chart-30). [1] The quadrangle covers all the area of Mars south of 65°, including the South polar ice cap, and its ...
1995 photo of Mars showing approximate size of the polar caps. The planet Mars has two permanent polar ice caps of water ice and some dry ice (frozen carbon dioxide, CO 2).Above kilometer-thick layers of water ice permafrost, slabs of dry ice are deposited during a pole's winter, [1] [2] lying in continuous darkness, causing 25–30% of the atmosphere being deposited annually at either of the ...
The "Water Strategy" was "to explore and study Mars in three areas: - Evidence of past or present life, - Climate (weather, processes, and history), - Resources (environment and utilization)." All three areas were seen as intimately connected to water.
Geology of Mars – Scientific study of the surface, crust, and interior of the planet Mars; Groundwater on Mars – Water held in permeable ground; Impact crater – Circular depression in a solid astronomical body formed by the impact of a smaller object; Lakes on Mars – Former Bodies of Water on Mars; Scientific information from the Mars ...
The current Venusian atmosphere has only ~200 mg/kg H 2 O(g) in its atmosphere and the pressure and temperature regime makes water unstable on its surface. Nevertheless, assuming that early Venus's H 2 O had a ratio between deuterium (heavy hydrogen, 2H) and hydrogen (1H) similar to Earth's Vienna Standard Mean Ocean Water of 1.6×10 −4, [7] the current D/H ratio in the Venusian atmosphere ...
Locate water-ice and carbon dioxide condensate clouds and determine their temperature, height and condensate abundance. Study the growth, retreat and total energy balance of the polar cap deposits. Measure the thermophysical properties of the Martian surface (thermal inertia, albedo) used to derive surface particle size and rock abundance.