13. January 2020
Mars Express mission

Im­pres­sive cloud for­ma­tions over Mars' north­ern po­lar ice cap

View of part of the northern polar ice cap
View of part of the north­ern po­lar ice cap
Image 1/3, Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

View of part of the northern polar ice cap

Char­ac­ter­is­tic fea­tures of the north po­lar cap in­clude dark fis­sures and val­leys that spi­ral out­ward from the cen­tre of the po­lar re­gion in a coun­ter­clock­wise di­rec­tion. Strat­i­fi­ca­tion is vis­i­ble on the steep slopes, rem­i­nis­cent of tree rings. This at­tests to sea­son­al changes in ice de­posits and dust cov­er due to Mar­tian storms. By ex­am­in­ing these lay­er pro­files, sci­en­tists hope to gain in­sights in­to the de­vel­op­ment of the Mar­tian cli­mate. The per­ma­nent wa­ter ice cov­er at the north pole is over two kilo­me­tres thick in places, while the sea­son­al car­bon diox­ide ice lay­ers are on­ly a few me­tres thick. Cloud for­ma­tions can be seen on the up to two-kilo­me­tre-high slopes of some of the val­leys; these are lo­cal dust storms that are sim­i­lar to fall winds.
3D-view of part of the Martian north pole
3D-view of part of the Mar­tian north pole
Image 2/3, Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

3D-view of part of the Martian north pole

Anaglyph im­ages can be pro­duced from da­ta ac­quired by the nadir chan­nel (ori­ent­ed ver­ti­cal­ly on­to the sur­face of Mars) of the HRSC in­stru­ment on board the ESA Mars Ex­press space­craft and one of the four oblique-view stereo chan­nels. When viewed with red-blue or red-green glass­es, these im­ages give a three-di­men­sion­al view of the land­scape. North is at the top right of the im­age. This view clear­ly shows the height dif­fer­ence of up to 2000 me­tres be­tween the dark clefts in the po­lar cap, which are sev­er­al hun­dred me­tres deep, and ice-cov­ered hills.
Topographic overview of the Martian north pole
To­po­graph­ic overview of the Mar­tian north pole
Image 3/3, Credit: MOLA Science Team / FU Berlin

Topographic overview of the Martian north pole

The HRSC cam­era sys­tem op­er­at­ed by DLR on board the ESA Mars Ex­press space­craft record­ed the marked strip dur­ing or­bit 3670. The land­scapes shown here are lo­cat­ed in the small­er rect­an­gle. Mars’ north­ern po­lar plain, al­so known as the Planum Bo­re­ale, spi­rals around the Red Plan­et's north pole.
  • Images acquired by HRSC show plumes of dust clouds over the ice cap at the Red Planet's north pole. Such observations of active atmospheric processes at the poles are rarely possible, and thus of great interest to scientists.
  • The characteristic features of the north polar cap include dark fissures and valleys that spiral outwards from the pole centre in a counterclockwise direction like a pinwheel.
  • On the steep slopes, stratification can be seen which, similarly to tree rings, reflects the seasonal change of ice deposition and dust cover caused by Martian storms.
  • Focus: Space, Mars, planetary research, exploration

These images show clouds of dust over our planetary neighbour's northern polar ice cap. They were acquired by the High Resolution Stereo Camera (HRSC), which is operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) and has been orbiting Mars on board the European Space Agency (ESA) Mars Express spacecraft since 2004. Such observations of active atmospheric processes at the Martian poles are rarely possible, and thus of great interest to scientists.

Like Earth, Mars has seasons. The Red Planet's polar axis is inclined at around 25 degrees, roughly the same as Earth's tilt. As such, Mars has the equivalent of our polar nights, without any sunlight in winter, and an Arctic or Antarctic summer, when the Sun does not set for months. Temperatures during the night and day vary just as dramatically on Mars, which affects the ice cover.

The appearance of Mars' north polar ice cap changes constantly over the course of a year. During the summer half, we see a permanent ice cap, part of which can be seen in this image. It essentially consists of water ice and has a diameter of approximately 1100 kilometres. It is estimated to have a volume of 1.6 million cubic kilometres, which equates to slightly over half the Greenland ice sheet, and is over two kilometres thick in places. Almost no impact craters can be seen on the ice, which indicates that the polar cap in its current form is not particularly old.

Dry ice allows the north polar cap to grow strongly over winter

During the winter half of the year, temperatures at the Martian north pole fall to below minus 125 degrees Celsius, and even in the temperate latitudes of the hemisphere in which it is winter, temperatures can drop to minus 40 degree Celsius or even lower during the day. At these low temperatures, a considerable proportion of the carbon dioxide from the thin Martian atmosphere condenses into ice ('dry ice') close to the poles and precipitates onto the surface. This enlarges the ice cap, forming what is known as the seasonal ice cap, consisting of a one- to two-metre-thick layer of carbon dioxide ice. This extends to 70 degrees north latitude. As a result, at this time of year the polar cap is often enshrouded in thick carbon dioxide clouds, making it difficult to observe from orbit. When spring sets in, the season layer of carbon dioxide ice quickly sublimates once again, turning directly into gas

The dark fissures between the gleaming white deposits of water ice are part of an impressive system of valleys that spiral outwards from the centre of the polar region in a counterclockwise direction. In places, these are up to two kilometres deep, making them similar in scale to the Grand Canyon, and cut through the layered deposits of the polar cap, which consists of a mixture of ice and dust. The transition between layers of ice and dust documents the development of the Martian climate over the last few millions of years, similarly to the annual rings of a tree.

Wind and dust storms carve deep valleys in the polar cap

The evaluation of radar data suggests that wind erosion is the driving force in the formation of spiral-shaped grooves. According to one theory, the valleys, with their cyclically formed steps, have been made by the impact of katabatic winds on the ice. Katabatic winds (from the Greek word katabasis, meaning descending) are downslope currents of cold, dense masses of air. They are caused by differences in density and form when, for example, cold, dry air flows from higher-lying surfaces of ice or snow into lower-lying areas with warmer, less dense air. These are commonly referred to as fall winds, as on Earth they often occur in the afternoon when the temperature differences are at their greatest, below glacier tongues.

In the case of Mars' polar cap, the air movement is directed radially outwards from the centre of the polar region and is also affected by the same Coriolis effect that exists on Earth. The Coriolis force, which acts upon gas masses in the atmosphere, is named after the French mathematician and engineer Gaspar de Coriolis (1792–1843) and is caused by the rotation of the planet, whereby the rotational velocity of a point on the surface decreases continuously from the equator (maximum) to the pole (zero). If air masses flow from temperate latitudes to the poles, they take the momentum of the planetary rotation with them and are deflected to the east. Even if 'slower' masses of air flow from the pole, they are 'overtaken' by the faster surface of the Earth and likewise deflected. This created spiral patters in atmospheric currents. The winds interact with the surface of Mars, creating the striking topographical spiral pattern of valleys and ridges.

The spectacular cloud formations in this HRSC image are small, local dust storms that are oriented perpendicular to the troughs and are particularly prevalent on the slopes of fissures that run towards the equator. This type of dust movement increases erosion and the regression of the steep slopes. Both sublimation and erosion due to the katabatic winds appear to be active aeolian processes that play a major role in the long-term alteration of valleys.

More images acquired by the High Resolution Stereo Camera can be found on DLR's Mars Express Flickr gallery.

Go to DLR's Mars Express mission site.

  • Image processing

    Systematic processing of the data acquired by HRSC took place at the DLR Institute of Planetary Research. From these data, staff in the Department of Planetary Sciences and Remote Sensing at the Freie Universität Berlin created the image products shown here. The image data were acquired by HRSC on 16 November 2016 during Mars Express orbit 3670. The image resolution is approximately 15 metres per pixel. The centre of the images is located at approximately 244 degrees east and 85 degrees north. The colour image was created using data from the nadir channel, the field of view of which is aligned perpendicular to the surface of Mars, and the colour channels of HRSC. The anaglyph, which provides a three-dimensional view of the landscape when viewed using red-green or red-blue glasses, was derived from data acquired by the nadir channel and the stereo channels.

  • The HRSC experiment on Mars Express

    The High Resolution Stereo Camera was developed by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) and built in collaboration with partners in industry (EADS Astrium, Lewicki Microelectronic GmbH and Jena-Optronik GmbH). The science team, which is headed by Principal Investigator (PI) Ralf Jaumann, consists of 50 co-investigators from 35 institutions in 11 countries. The camera is operated by the DLR Institute of Planetary Research in Berlin-Adlershof; it has been delivering high-resolution images of the Red Planet since 2004.
  • Elke Heinemann
    Ger­man Aerospace Cen­ter (DLR)

    Com­mu­ni­ca­tions and Me­dia Re­la­tions
    Telephone: +49 2203 601-2867
    Fax: +49 2203 601-3249
    Linder Höhe
    51147 Cologne
  • Prof.Dr. Ralf Jaumann
    Freie Uni­ver­sität Berlin
    In­sti­tute of Ge­o­log­i­cal Sci­ences
    Plan­e­tary Sci­ences and Re­mote Sens­ing
    Telephone: +49-172-2355864
    Malteserstr. 74-100
    12249 Berlin
  • Ulrich Köhler
    Ger­man Aerospace Cen­ter (DLR)
    In­sti­tute of Plan­e­tary Re­search
    Rutherfordstraße 2
    12489 Berlin

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