Baltis Vallis

Baltis Vallis

A radar mosaic from Magellan showing a 600 km long segment of Baltis Vallis.
Feature type Vallis
Coordinates 37°18′N 161°24′E / 37.3°N 161.4°E / 37.3; 161.4Coordinates: 37°18′N 161°24′E / 37.3°N 161.4°E / 37.3; 161.4
Diameter 6,000 km
Eponym Syrian word for planet Venus.

Baltis Vallis is a sinuous channel on Venus ranging from one to three kilometers wide and nearly 7,000 kilometers long, slightly longer than the Nile and the longest known channel of any kind in the solar system. It is thought that it once held a river of lava known as a lava channel.

The lava must have had a very low viscosity, possibly due to a carbonatite composition.[1] At the volcano Ol Doinyo Lengai in Tanzania, natrocarbonatite lava erupts at around 780 K (510 °C), not far above Venus's mean ambient temperature of 735 K (462 °C). Analysis of cross-sectional profiles (using brightness data from Magellan synthetic aperture radar images) indicates that while Baltis Vallis does have levees, primarily in its first 1500 km, and intrachannel ridges, mainly in the segment 1500 to 3000 km from the source, the feature is primarily erosional, with a bottom surface 20–100 m below the surrounding plains at 90% of the sites studied.[1] The average depths and widths of the channel are 46 ± 16 m and 2.2 ± 0.4 km, respectively.[1]

The channel is located in an area consisting entirely of plains and wrinkle ridges. The topography of the channel undulates, with some stretches travelling uphill, suggesting that various regions have uplifted and subsided since the channel formed.

Both ends of the channel are obscured, however, so its original length is unknown. The channel was initially discovered by the Soviet Venera 15 and 16 orbiters which, in spite of their one-kilometer resolution, detected more than 1,000 kilometers (620 mi) of the channel. These channel-like features are common on the plains of Venus. In some places they appear to have been formed by lava which may have melted or thermally eroded a path over the plains' surface. Most are 1 to 3 kilometers (0.6 to 2 miles) wide. They resemble terrestrial meandering rivers in some aspects, with meanders, cutoff bows and abandoned channel segments. However, Venus channels are not as tightly sinuous as terrestrial rivers. Most are partly buried by younger lava plains, making their sources difficult to identify. A few have vast radar-dark plains units associated with them, suggesting large flow volumes. These channels with large deposits appear to be older than other channel types, as they are crossed by fractures and wrinkle ridges, and are often buried by other volcanic materials. In addition, they appear to run both upslope and downslope, suggesting that the plains were warped by regional tectonism after channel formation.

References

  1. 1 2 3 Oshigami, S.; Namiki, N. (Sep 2007). "Cross-sectional profiles of Baltis Vallis channel on Venus: Reconstructions from Magellan SAR brightness data". Icarus. 190 (1): 1–14. Bibcode:2007Icar..190....1O. doi:10.1016/j.icarus.2007.03.011.
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