At deeper levels of the impact where the material is not ejected, tensional stresses in the release waves are lower. As a result, fracturing is less pronounced, excavation flow velocities are lower, and the excavation flow lines themselves are not oriented to eject material beyond the crater rim. This region forms a displaced zone in which material is driven downward and outward more or less coherently. Both zones in the transient crater continue to expand, accompanied by the uplift of near-surface rocks to form the transient crater rim. However, these waves continually loose energy by deforming and ejecting the target rocks through which they pass. Eventually, a point is reached at which the shock and release waves can no longer excavate or displace target rock. At that point the growth of the transient crater ceases. (French, 1998).


Crater Giordano Bruno, located on the far side of our moon, illustrates a “classic” rim shape.. – Image courtesy of JAXA/SELENE

It is estimated that it was a 1-3 km wide asteroid that impacted at the Moon’s northeast limb to form the 22 km diameter Giordano Bruno Crater. When viewed from orbit, Giordano Bruno is at the center of a symmetrical ray system of ejecta that has a higher albedo than the surrounding surface, implying a high angle impact. The ray material extends for over 150 kilometers and has not been significantly darkened by space erosion.

As illustrated at the Giordano Bruno Crater, what remains when the growth of the transient crater stops is a depression with an upraised rim, and the modification stage begins. The exposed rim, walls, and floor define the so-called apparent crater. At the rim, there is an overturned flap of ejected target materials, which displays inverted stratigraphy, with respect to the original target materials (Grieve, 2002). An overturned rim sequence is now recognized as one of the hallmarks of an impact crater.


Barringer Crater is one of the few craters on this planet with a remaining crater rim. The crater has slightly polygonal sides and the rim rises nearly 50 m above the surrounding plain. Beyond the rim are low mounds of material ejected by the impact.

The rim of the 1.19 kilometre diameter Barringer Crater is still well defined, even after approximately 49 thousand years of erosion. It has been estimated that the first two stages of the cratering process (time from initial contact of the impactor until the end of the excavation stage) here at Barringer took approximately 6 seconds! Almost 63 million cubic metres were evacuated from this area in that time to form the crater. The height of the rim over the surrounding plain is 36 – 61 metres. Investigations around this rim confirmed an “overturned rim sequence”.


The rim of the Pingualuit Impact Structure rises approximately 160 metres over the surrounding tundra and still retains its basic shape after more than 1 million years of erosion.

My 11 kilometre exploration hike around the rim of the 3.44 kilometre diameter Pingualuit Impact Structure took most of a day and was not one of the easiest of hikes that I have experienced. Along the lip of the rim there were frequent gullies that we had to traverse. This image gives you a good size perspective, as the people leading the hike are just visible on the rim in the far distance.


The unique geology at the crater rim of the St. Martin Crater possibly causing this extreme change in the flow direction of the Dauphin River.

The rim of the St. Martin complex crater is buried by over 100 metres of Jurassic red beds and glacial drift. It is my hypothesis that the cause of this extreme diversion of the Dauphin River at the rim of the St. Martin crater is the differential sagging of the outlaying bedrock compared to the breccia within the impact structure. To my knowledge, there is no published report that explains the cause of this river’s diversion at this specific location. The Dauphin River then follows this rim to the East and flows into Lake Winnipeg.