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The Poles of Venus - Windows to the Universe

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Learn about planets outside our solar system through Exoplanets and Alien Solar Systems by Tahir Yaqoob, Ph.D., a book in our online store book collection.
This radar map of the northern hemisphere of Venus shows how the surface might look if we could peer through the planet's thick atmosphere. The North Pole is at the center of the image. The bright region just below the center is Maxwell Montes, the highest mountain chain on Venus.
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Image courtesy of NASA/JPL.

The Poles of Venus

Would you expect to find ice caps and snow fields on Venus? Not likely! Venus is the hottest planet in our Solar System, and those high temperatures extend right on up to the poles. Though there aren't any Venusian polar ice caps, there are interesting features at the planet's poles. Some rugged mountain ranges, as well as the tallest mountain on the planet, lie at high latitudes on Venus. The polar atmosphere contains swirling double vortices of winds and clouds.

Although we cannot peer through the thick clouds of Venus to see its surface, scientists have mapped its features using radar. Venus has two "continents" - large areas of raised land. One of these, Ishtar Terra, is about the size of Australia and lies near the North Pole. The highest mountain chain on Venus, Maxwell Montes, is on Ishtar Terra. The mountains are located at a latitude similar to Alaska and tower 11 km (6.6 miles) above the average surface height of Venus.

Some of the lowlands on Venus are crossed by ridge belts which are up to hundreds of kilometers wide and thousands long. The ridge belts rise several kilometers above the surrounding lowlands. There are two major concentrations of these belts: one in Lavinia Planitia near the South Pole, and another next to Atalanta Planitia by the North Pole.

The surface temperatures on Venus are extremely high, around 464 C (867 F). The incredibly dense atmosphere spreads this heat evenly over the surface and keeps it very steady through time. The nighttime side of the planet is just as hot as daytime side, and poles of Venus are just as scorching hot as the equator. The spin axis of Venus is tilted a mild 3 (compared to Earth's 23). Due to this minimal tilt and the thick atmosphere, there are no seasons on Venus. Wherever you go... and whenever you go... on Venus, you can count on it being hot!

There are swirling double vortices in the Venusian polar atmosphere above each of the poles. Polar vortices form on other planets, including Earth and Saturn. However, the double-vortex structures seem unique to Venus.

Last modified May 18, 2009 by Randy Russell.

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Windows to the Universe, a project of the National Earth Science Teachers Association, is sponsored in part by the National Science Foundation and NASA, our Founding Partners (the American Geophysical Union and American Geosciences Institute) as well as through Institutional, Contributing, and Affiliate Partners, individual memberships and generous donors. Thank you for your support! NASA AGU AGI NSF