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  2. Glaciers on Mars - Wikipedia

    en.wikipedia.org/wiki/Glaciers_on_Mars

    It is thought that ice accumulated when Mars' orbital tilt was very different from the present (the axis the planet spins on has considerable "wobble," meaning its angle changes over time). [39] [40] [41] A few million years ago, the tilt of the axis of Mars was 45 degrees instead of its present 25 degrees. Its tilt, also called obliquity ...

  3. Martian polar ice caps - Wikipedia

    en.wikipedia.org/wiki/Martian_polar_ice_caps

    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 ...

  4. Geology of Mars - Wikipedia

    en.wikipedia.org/wiki/Geology_of_Mars

    Mars also has an atmosphere that plays a role in ejecta emplacement and subsequent erosion. Moreover, Mars has a rate of volcanic and tectonic activity low enough that ancient, eroded craters are still preserved, yet high enough to have resurfaced large areas, producing a diverse range of crater populations of widely differing ages.

  5. Common surface features of Mars - Wikipedia

    en.wikipedia.org/.../Common_surface_features_of_Mars

    After the dry ice is gone, new channels are visible. These gullies may be caused by blocks of dry ice moving down the steep slope or perhaps from dry ice starts the sand moving. [16] In the thin atmosphere of mars, dry ice will expel carbon dioxide with vigor. [17] [14]

  6. Martian dichotomy - Wikipedia

    en.wikipedia.org/wiki/Martian_dichotomy

    Geology of Mars – Scientific study of the surface, crust, and interior of the planet Mars; Glacier – Persistent body of ice that moves downhill under its own weight; Glaciers on Mars – Extraterrestrial bodies of ice; Lobate debris apron – Geological features on Mars; Nilosyrtis Mensae – Fretted terrain in the Casius quadrangle on Mars

  7. Martian chaos terrain - Wikipedia

    en.wikipedia.org/wiki/Martian_chaos_terrain

    These ice ages are caused by the frequent large changes in the tilt of the planet. [24] The tilt of the spin axis of Mars is highly variable due to the lack of a large moon. [25] [26] [27] Observations of many craters have shown that many craters are mostly full of sediments—ice could be one of the sediments. Many craters appear to be very ...

  8. Gullies on Mars - Wikipedia

    en.wikipedia.org/wiki/Gullies_on_Mars

    After the dry ice is gone, new channels are visible. These gullies may be caused by blocks of dry ice moving down the steep slope or perhaps from dry ice starts the sand moving. [89] [90] In the thin atmosphere of mars, dry ice will expel carbon dioxide with vigor. [91] [87]

  9. Evidence of water on Mars found by Mars Reconnaissance ...

    en.wikipedia.org/wiki/Evidence_of_water_on_Mars...

    Research, reported in the journal Science in September 2009, [91] demonstrated that some new craters on Mars show exposed, pure, water ice. After a time, the ice disappears, evaporating into the atmosphere. The ice is only a few feet deep. The ice was confirmed with the Compact Imaging Spectrometer (CRISM) on board the Mars Reconnaissance ...