In June 2019 the High Resolution Stereo Camera (HRSC) captured a number of global images of Mars. The view shown in the main image stretches from the North Pole to the heavily cratered highlands around the Martian equator and far into the southern hemisphere. HRSC, which is on board the European Space Agency (ESA) Mars Express spacecraft, was developed by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR). It has been operated by the DLR Institute of Planetary Research for more than 16 years. The Institute also processes the data acquired by the camera system. From these data, specialists in planetology and remote sensing at the Freie Universität Berlin have created the images shown here.

The upper part of this striking global view of Mars shows the northern hemisphere and the North Pole ice cap in winter. A thin veil of clouds stretches from there across the adjoining deep valleys, some of which are covered with dark sand. A prominent escarpment is visible in the image. This marks the border between Mars’ northern lowlands and its southern highlands. Dark sands also cover some areas of the crater-strewn highlands. In the extreme south (bottom) of the image, part of the Hellas impact crater is visible, covered by white clouds. The view of the planet is slightly ‘tilted’ towards the south, allowing the North Pole to be seen, but it only extends down to 40 degrees south. The South Pole is therefore not visible. From pole to pole, Mars measures 6752 kilometres; the image shown here covers just under 5000 kilometres of that distance.

Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

Download the image in the Mulitimedia area

Different climate zones and major geographical regions

During winter in the northern hemisphere, the intense cold causes significant quantities of carbon dioxide to precipitate out of the atmosphere above the North Pole; it forms a thin layer above the permanent polar cap, which otherwise consists predominantly of water ice. This ice cover then extends down to approximately 50 degrees north. The water vapour content in the Martian atmosphere, which could potentially freeze to form water ice and fall to the surface as snow or ice, is extremely low. It averages just 0.03 percent and is subject to strong fluctuations. Carbon dioxide, on the other hand, is the major constituent of the Martian atmosphere, accounting for 95 percent of the gases.

The image data were acquired at the beginning of spring in the north; the polar night at the North Pole was over and the polar cap, which had grown during the winter, is gradually beginning to recede. This growth and shrinkage can also be seen at the southern polar cap. The thin white band of cloud (probably composed of water ice crystals) is one of many that appear over the northern hemisphere at this time of year.

Why are the Martian highlands and lowlands so drastically different?

The reddish plains of Arabia Terra and Terra Sabaea in the centre of the image are notable for the presence of many large impact craters, indicating that they are among the oldest regions on Mars. Along their northern border is a striking escarpment, with a difference of several kilometres in height. This separates the flat, barely cratered plains of the northern lowlands from the southern highlands, which have many more craters. This remarkable change in terrain, referred to as the Martian dichotomy, marks a fundamental topographical and regional division on Mars. This is reflected, most importantly, in the different crust thicknesses, but also extends to the magnetic properties of the crust and its gravitational field. There is still a certain amount of scientific debate over how this crust dichotomy came about. It could have originated from ‘endogenous’ forces in the Martian interior and thus been caused by mantle convection or tectonics. If ‘exogenous’ (external) forces were responsible, this effect could perhaps be traced back to one or more major asteroid impacts.



The intensely rugged landscape at the dichotomous boundary has been severely eroded over millions of years, and is now characterised by numerous tectonic faults, mesas and river valleys. Observations have revealed that fluvial, aeolian and, in particular, glacial processes have altered the transition zone. Analysis of the image data suggests that there may have been several episodes of glacial activity during the evolution of Mars.

How winds have shaped the surface of Mars

Geological processes (volcanism, tectonics, water and ice activity) have come to a standstill on Mars. Today, changes that can be observed on the surface are primarily caused by the wind-induced displacement of dark sands. While these sands, which are of volcanic origin, form vast dune fields in depressions such as impact craters, they are also often deposited over other large areas, which causes parts of the planetary surface to have a dark appearance. The displacement of dunes can be observed over a timeframe of one to two years using high-resolution image data.



In contrast, shifts in the wide-area layers of sand take much longer. When the Italian astronomer Giovanni Schiaparelli (1835–1910) first mapped Mars in 1877, during a period when observation conditions were particularly favourable, changes in the distribution of light and dark surfaces on Mars could be monitored over a longer period. It was then believed that the movement of the dark areas were caused by seasonal changes in vegetation cover. This was one source of the belief that there was life on Mars.

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