Impact Craters -->
Large impact craters with diameters a few to 280 km are visible in the fractured plains. Smaller craters are not found since smaller meteorites never make it to the ground. Typical crater features seen: rough radar-bright ejecta surrounds the perimeter of the craters; terraced inner walls; and large central peaks. Crater floors appear dark because they are smooth, flooded by lava. There are nearly 1000 evenly spaced (surface is all the same age) craters on Venus. The low number ages the current surface at 800 m.y.o. With no weathering, global tectonics must be capable of restoring the entire surface.

<-- Large scale Tectonic Features
Several tectonic events formed this complex terrain, which is part of the interior of Ovda Regio. An underlying fabric of ridges and valleys are spaced 10-20 km (6-12 mi) apart and may have been caused by compression of the crust at right angles to the ridge. The largest valleys, particularly the 20 km (12 mi) wide valley extending across the image, were filled with dark material, probably lava. The complexity of Ovda Regio attests to a long history of tectonic deformation.

Corona -->
Located in Lada Terra, Selu Corona measures 350 km (210 mi) in diameter. Coronae are circular to elliptical features marked by a ring of concentric ridges, and are thought to result from the flow of heat in the planet's interior. As hot material rises, it weakens the upper layers of the crust, causing the surface to dome upwards. Then as the region cools, the dome begins to subside. As the upper layers rise and fall, they are subjected to stresses that crack the surface, creating both circular and radial fractures.