Eastern scarp of Olympus Mons

The HRSC obtained these images during orbit 1089 with a ground resolution of approximately 11 metres per pixel. The image is centred at 17.5° North and 230.5° East. The scarp is up to six kilometres high in places.

The surface of the summit plateau’s eastern flank shows lava flows that have are several kilometres long and a few hundred metres wide.

Age determinations show that they are up to 200 million years old, in some places even older, indicating episodic geological activity.

The lowland plains, seen here in the eastern part of the image (bottom), typically have a smooth surface.

Several channel-like features are visible which form a broad network composed of intersecting and ‘anastomosing’* channels that are several kilometres long and up to 40 metres deep. (*Anastomising means branching extensively and crossing over one another, like veins on the back of your hand.)

Several incisions suggest a tectonic control, others show streamlined islands and terraced walls suggesting outflow activity.

Age determinations show that the network-bearing area was geologically active as recent as 30 million years ago.

Between the edge of the lowland plains and the bottom of the volcano slope, there are ‘wrinkle ridges’ which are interpreted as the result of compressional deformation. In some places, wrinkle ridges border the arch-like terraces at the foot of the volcano slope.

The colour scenes have been derived from the three HRSC-colour channels and the nadir channel.

The perspective views have been calculated from the digital terrain model derived from the stereo channels.

The 3D anaglyph image was calculated from the nadir and one stereo channel. Image resolution has been decreased for use on the internet.

For more information on Mars Express HRSC images, you might like to read our updated 'Frequently Asked Questions'.