[1] With a diameter of 716 km it is the second-largest impact basin on the planet, after Caloris,[2] and is one of the larger craters in the Solar System.

The former occupies a part of the basin's floor near its northern margin forming an incomplete ring about 130 km (81 mi) wide.

The smooth plains are intersected by a system of wrinkle-ridges and troughs, named Borobudur Fossae, both having radial or concentric shapes.

Some radial troughs closely follow wrinkle ridges forming a unique wheel spoke pattern.

[2] Rembrandt basin is cross-cut by a large lobate scarp running from the southwest to the north, named Enterprise Rupes.

It is about 600 km (370 mi) long and belongs to the global system of scarps, which covers the entire surface of Mercury.

Those impact craters, which formed after the end of volcanism, indicate that in the center of Rembrandt lava, layers can be as thick as 2 km (1.2 mi).

The basin probably formed near the end of the Late Heavy Bombardment of the inner Solar System about 3.9 billion years ago.

Light-colored lavas filled the inner part of Rembrandt causing it to subside, which led to the contraction of the basin's floor and formation of wrinkle ridges.

[2] The latest episode of tectonic activity led to the formation of the lobate scarp, which actually runs tangentially to the ring of wrinkle ridges.