Radar image of Maxwell Montes
|Feature type||Mountain range|
|Diameter||797 kilometres (495 mi)|
|Eponym||James Clerk Maxwell|
Located on Ishtar Terra, the more northern of the planet's two major highlands, Maxwell Montes is 11 kilometres (6.8 mi) high. It rises about 6.4 kilometres (4 mi) above and to the east of Lakshmi Planum, and is about 853 kilometres (530 mi) long by 700 kilometres (435 mi) wide. The western slopes are very steep, whereas the eastern slopes descend gradually into Fortuna Tessera. Due to its elevation it is the coolest (about 380 °C or 716 °F) and least pressurised (about 45 bar or 44 atm) location on the surface of Venus.
Origins and geology
The origin of the Lakshmi Planum and the mountain belts such as Maxwell Montes is controversial. One theory suggests they formed over a hot plume of material rising from the interior of the planet, while another says the region is being compressed (pushed together) from all sides, resulting in material descending into the interior of the planet. The broad ridges and valleys making up Maxwell Montes and Fortuna Tessera suggest that the topography resulted from compression. The parallel ridges and valleys were cut by later extensional faults. The extreme height of Maxwell Montes in relation to other compressional mountain ranges around Lakshmi Planum suggests that its origin is more complex.
Most of Maxwell Montes has a bright radar return which is common on Venus at high altitudes. This phenomenon is thought to result from the presence of a mineral, possibly a metallic snow. Early suggestions included pyrite and tellurium; more recently, lead sulfide and bismuth sulfide have been proposed.
Radar mapping and naming
By using radar to probe through the permanent and thick clouds in the Venusian atmosphere and make observations of the surface, scientists at the American Arecibo Radio Telescope in Puerto Rico discovered the extensive highland on Venus that came to be called Maxwell Montes in 1967.
In 1978, the space probe Pioneer Venus 1 went into orbit around Venus for the purpose of making radar observations of the Venusian surface. These observations made possible the creation of the first topographic map of the surface of Venus, and confirmed that a point within Maxwell Montes is the highest point above the average level of the planet's surface.
The name, originally given by Ray Jurgens in 1970 on the urging of Tommy Gold, was approved by the International Astronomical Union's Working Group for Planetary System Nomenclature (IAU/WGPSN) between 1976 and 1979.
- Jones, Tom; Stofan, Ellen (2008). Planetology : Unlocking the secrets of the solar system. Washington, D.C.: National Geographic Society. p. 74. ISBN 978-1-4262-0121-9.
- "PIA00149: Venus - Maxwell Montes and Cleopatra Crater". NASA Planetary Photojournal. Retrieved 2009-06-11.
- Basilevsky A. T., Head J. W. (2003). "The surface of Venus". Reports on Progress in Physics. 66 (10): 1699–1734. Bibcode:2003RPPh...66.1699B. doi:10.1088/0034-4885/66/10/R04.
- McGill G. E.; Stofan E. R.; Smrekar S. E. (2010). "Venus tectonics". In T. R. Watters; R. A. Schultz. Planetary Tectonics. Cambridge University Press. pp. 81–120. ISBN 978-0-521-76573-2.
- "The Magellan Venus Explorer's Guide - The Geology of Venus". NASA JPL. Retrieved 2009-06-11.
- Otten, Carolyn Jones (2004-02-10). "'Heavy metal' snow on Venus is lead sulfide". Newsroom. Washington University in Saint Louis. Retrieved 2012-12-10.
- Butrica, Andrew J., SP-4218 To See the Unseen, Chapter 5: Normal Science, NASA, 1996
- "Pioneer Venus 1, Orbiter and Multiprobe spacecraft". NASA. Retrieved 2009-06-11.
- "EXTREME Space Venus". NASA. Retrieved 2009-06-11.
- Butrica, Andrew J., SP-4218 To See the Unseen, Chapter 6: Pioneering on Venus and Mars, NASA, 1996