Noachis is so densely covered with impact craters that it is considered among the oldest landforms on Mars—hence the term "Noachian" for one of the earliest time periods in martian history.

Much of the surface in Noachis quadrangle shows a scalloped topography where the disappearance of ground ice has left depressions.

[5][6] This mantle material probably fell from the air as ice formed on dust when the climate was different due to changes in the tilt of the Mars pole.

A study published in Icarus, found that the landforms of scalloped topography can be made by the subsurface loss of water ice by sublimation under current Martian climate conditions.

Their model predicts similar shapes when the ground has large amounts of pure ice, up to many tens of meters in depth.

When a dust devil goes by it blows away the coating and exposes the underlying dark surface creating tracks.

[16] TA study that combined data from the High Resolution Stereo Camera (HRSC) and the Mars Orbiter Camera (MOC) found that some large dust devils on Mars have a diameter of 700 meters and last at least 26 minutes.

[18] The image below of Russel Crater shows changes in dust devil tracks over a period of only three months, as documented by HiRISE.

Recently, because changes in gullies have been seen since HiRISE has been orbiting Mars, it is thought that they may be formed by chunks of dry ice moving down slope during spring time.

A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas.

They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas.