Splashdown! Crashing into martian mud

September 14, 2017
Perspective view of a 32 km-wide impact crater north of the Hellas basin that formed at time when the martian environment was much wetter, as seen in the fluidised nature of the debris excavated from it. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

An impactor smashing into an ice-rich surface gave rise to the complex flow features around this ancient crater on Mars.

Impacts of comets and asteroids have shaped the surfaces of and moons over the Solar System's 4.6 billion year history, and can reveal at the time of their formation.

During an , the energy transferred to the ground goes into melting and vapourising the impactor and parts of the surface, as well as excavating vast amounts of material from the ground, throwing it out onto the surrounding terrain as a blanket of debris.

The characteristics of the ejected material can provide clues as to the conditions of the planet's surface and its general environment.

The 32 km-wide crater seen centre-stage in this image clearly formed at a time when water or ice was present near the surface. The energy of the impact heated up the water-rich sub-, allowing it to flow more easily, leading to the 'fluidised' nature of the ejecta blanket.

The periphery of the lobes of excavated material often displays a raised ridge: as the flow slowed, the debris behind it piled up, pushing up the material at its periphery into ramparts.

Colour view of crater north of the Hellas basin. The crater is 32 km-wide and was formed at time when the martian environment was much wetter, as seen in the fluidised nature of the debris excavated from it. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

Many craters on Mars show this pattern, sometimes with of ejecta. Here, up to three layers of ejecta lobes can be identified, some of them terminating in ramparts. Multiple layer ejecta deposits can result from a combination of impact into a buried layer of water-rich ground, and interaction of ejected material with the atmosphere.

The scene is located north of the Hellas impact basin, one of the largest in the entire Solar System at 2300 km. The region is in an area that is suspected to be the former drainage basin of a lake.

Small channels can also be seen to the south in the main image (left), providing more evidence of the region's watery past.

This image shows the relative heights of a cratered region north of the Hellas Basin on Mars. As indicated in the key at top right, whites and browns/reds represent the highest terrain, while blue/purple is the lowest. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

Explore further: Remnants of a mega-flood on Mars

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