These low-lying plains, particularly in the western portion, are characterized by apparent volcanic source vents and broad regions of bright, dark, and mottled deposits.

[1] The types, numbers, and patterns of mapped tectonic features and small volcanic landforms in the region provide important detail in the interpretation and evolution of venusian landscape.

[2] By using Pioneer Venus, Goldstone, and Arecibo data, these regions have been interpreted as widespread superposed flows that originated from the source vents.

[5] Complex ridge terrain in Guinevere Planitia consists of embayed remnants of material that have undergone extensive deformation.

Wrinkle ridges can be viewed as the purple fill in figure C. These outcrops dominate the low-lying region and are marked with yellow lines that represent major trends.

Relative age relationships both within and between the major eruptive centers are difficult to determine due to the complex nature in which these flows coalesce and inter-finger.

Tuli rises an average of 600 m above its surroundings, and its flanks consist of a series of lobate, narrow flows which radiate from the summit region.

At the summit, radial flows surround a small shield or cone with a central pit roughly 12 km in diameter.

On the southern flank of Var Mons lies narrow, lobate flows which extend for ~500 km where they overlie dark, ridged plains.

North of the summit extends a prominent rift zone that stretches a distance of 250 km where it terminates in a cluster of ring structures.