Ovda Regio is a Venusian crustal plateau located near the equator in the western highland region of Aphrodite Terra that stretches from 10°N to 15°S and 50°E to 110°E.

Known as the largest crustal plateau in Venus, the regio covers an area of approximately 15,000,000 square kilometres (5,800,000 sq mi)[1] and is bounded by regional plains to the north, Salus Tessera to the west, Thetis Regio to the east, and Kuanja as well as Ix Chel chasmata to the south.

[2] The crustal plateau serves as a place to hold the localized tessera terrains in the planet, which makes up roughly 8% of Venus' surface area.

Synthetic aperture radar (SAR) images from the NASA Magellan mission have been analyzed to recognize the distribution of its structural features.

The folds observed in this part of the Regio are concentric, associated with plunges, and share a common axis that is trending in an east–west fashion.

Other structural features observed in this part of Ovda are imbricate stack and duplex formation on the southern margin.

Some of the ribbons structures on this part of Ovda are quite difficult to interpret due to the SAR images' limited resolution.

Furthermore, the last phase occurred when the extensional events continuously carried out the deformed structures from the plateau and affecting the volcanic units.

[11] This second model describes the upwelling of a mantle flow (plume) that accommodates the formation of crustal thickening by magmatic underplating and volcanic activities associated with the thin lithosphere.

The first issue is that scientists are not confident that meteor impacts have the capabilities to melt a significant portion of the planet's lithosphere and generate enough magma that would cause isostasy.