File:Saturn Kelvin Helmholtz.jpg
Summary
A <a href="//commons.wikimedia.org/w/index.php?title=Kelvin-Helmholtz_instability&action=edit&redlink=1" class="new" title="Kelvin-Helmholtz instability (page does not exist)">Kelvin-Helmholtz instability</a> on <a href="//commons.wikimedia.org/wiki/Saturn_(planet)" title="Saturn (planet)">Saturn</a>, caused by the interaction between two bands of the planet's atmosphere. Image from the <a href="//commons.wikimedia.org/w/index.php?title=Cassini-Huygens_Mission&action=edit&redlink=1" class="new" title="Cassini-Huygens Mission (page does not exist)">Cassini</a> probe. Caption from NASA's press release: This turbulent boundary between two latitudinal bands in Saturn's atmosphere curls repeatedly along its edge in this Cassini image. This pattern is an example of a Kelvin-Helmholtz instability, which occurs when two fluids of different density flow past each other at different speeds. This type of phenomenon should be fairly common on the <a href="//commons.wikimedia.org/w/index.php?title=Gas_giant&action=edit&redlink=1" class="new" title="Gas giant (page does not exist)">gas giant</a> planets given their alternating jets and the different temperatures in their belts and zones. The image was taken with the Cassini spacecraft narrow angle camera on <a href="//commons.wikimedia.org/wiki/October_9" title="October 9">October 9</a>, <a href="//commons.wikimedia.org/wiki/2004" title="2004">2004</a>, at a distance of 5.9 million kilometers (3.7 million miles) from Saturn through a filter sensitive to wavelengths of <a href="//commons.wikimedia.org/w/index.php?title=Infrared&action=edit&redlink=1" class="new" title="Infrared (page does not exist)">infrared</a> light centered at 889 nanometers. The image scale is 69 kilometers (43 miles) per pixel.
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 15:31, 17 January 2017 | | 550 × 315 (12 KB) | 127.0.0.1 (talk) | <p>A <a href="//commons.wikimedia.org/w/index.php?title=Kelvin-Helmholtz_instability&action=edit&redlink=1" class="new" title="Kelvin-Helmholtz instability (page does not exist)">Kelvin-Helmholtz instability</a> on <a href="//commons.wikimedia.org/wiki/Saturn_(planet)" title="Saturn (planet)">Saturn</a>, caused by the interaction between two bands of the planet's atmosphere. Image from the <a href="//commons.wikimedia.org/w/index.php?title=Cassini-Huygens_Mission&action=edit&redlink=1" class="new" title="Cassini-Huygens Mission (page does not exist)">Cassini</a> probe. Caption from NASA's press release: This turbulent boundary between two latitudinal bands in Saturn's atmosphere curls repeatedly along its edge in this Cassini image. This pattern is an example of a Kelvin-Helmholtz instability, which occurs when two fluids of different density flow past each other at different speeds. This type of phenomenon should be fairly common on the <a href="//commons.wikimedia.org/w/index.php?title=Gas_giant&action=edit&redlink=1" class="new" title="Gas giant (page does not exist)">gas giant</a> planets given their alternating jets and the different temperatures in their belts and zones. The image was taken with the Cassini spacecraft narrow angle camera on <a href="//commons.wikimedia.org/wiki/October_9" title="October 9">October 9</a>, <a href="//commons.wikimedia.org/wiki/2004" title="2004">2004</a>, at a distance of 5.9 million kilometers (3.7 million miles) from Saturn through a filter sensitive to wavelengths of <a href="//commons.wikimedia.org/w/index.php?title=Infrared&action=edit&redlink=1" class="new" title="Infrared (page does not exist)">infrared</a> light centered at 889 nanometers. The image scale is 69 kilometers (43 miles) per pixel. </p> |
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