page_title: Planum Boreum
section_title: Ice cap
hierarchical_section_title: Planum Boreum / Features / Ice cap
caption_attribution_description: English: The North Polar layered deposits are a 3-kilometer thick stack of dusty water ice layers that are about 1000 kilometers across. The layers record information about climate stretching back a few million years into Martian history. In many locations erosion has created scarps and troughs that expose this layering. The tan colored layers are the dusty water ice of the polar layered deposits; however a section of bluish layers are is visible below them. These bluish layers contain sand-sized rock fragments that likely formed a large polar dunefield before the overlying dusty ice was deposited. The lack of a polar ice cap in this past epoch attests to the variability of the Martian climate, which undergoes larger changes over time than that of the Earth. The map is projected here at a scale of 50 centimeters (19.6 inches) per pixel. [The original image scale is 63.6 centimeters (25 inches) per pixel (with 2 x 2 binning); objects on the order of 191 centimeters (75.2 inches) across are resolved.] North is up. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace &amp; Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. Depicted width of this image: about 1300 meters (0.8 miles), per scaled images [1], [2]
context_page_description: Planum Boreum is the northern polar plain on Mars. It extends northward from roughly 80°N and is centered at 88.0°N 15.0°E. Surrounding the high polar plain is a flat and featureless lowland plain called Vastitas Borealis which extends for approximately 1500 kilometres southwards, dominating the northern hemisphere.
context_section_description: Planum Boreum is home to a permanent ice cap consisting mainly of water ice (with a 1 m thick veneer of carbon dioxide ice during the winter). It has a volume of 1.2 million cubic kilometres and covers an area equivalent to about 1.5 times the size of Texas. It has a radius of 600 km. The maximum depth of the cap is 3 km.
  The spiral troughs in the ice cap are formed by katabatic winds that entrain surface ice eroded from the equator-facing sides of the troughs, likely aided by solar ablation (sublimation), which is then redeposited on the colder pole-facing slopes. The troughs are roughly perpendicular to the wind direction, which is shifted by the Coriolis effect, leading to the spiral pattern. The troughs gradually migrate towards the pole over time; the central troughs have moved about 65 km in the last 2 million years. Chasma Boreale is a canyon-like feature older than the troughs, and in contrast is aligned parallel to the wind direction.
  The surface composition of the northern ice cap in middle spring (after a winter's accumulation of seasonal dry ice) has been studied from orbit. The outer edges of the ice cap are contaminated with dust (0.15% by weight) and are mostly water ice. As one moves toward the pole, the surface water ice content decreases and is replaced by dry ice. The purity of the ice also increases. At the pole, the surface seasonal ice consists of essentially pure dry ice with little dust content and 30 parts per million of water ice.
  The Phoenix lander, launched in 2007, arrived at Mars in May 2008 and successfully landed in the Vastitas Borealis region of the planet on May 25, 2008. The north polar cap of Mars has been proposed as a landing site for a human Mars expedition by Geoffrey A. Landis and by Charles Cockell.
caption: False color HiRISE view of water ice layers in Olympia Rupes, believed by scientists to be preserving climate conditions of Mars dating back millions of years. Depicted width: 1.3 km (3⁄4 mi)
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