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Webcam on Mars Express surveys high-altitude clouds

(17 October 2017 - ESA) An unprecedented catalogue of more than 21 000 images taken by a webcam on ESA’s Mars Express is proving its worth as a science instrument, providing a global survey of unusual high-altitude cloud features on the Red Planet.

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Example of a sequence of images taken by ESA’s Mars Express Visual Monitoring Camera as a limb cloud came into view on 7 March 2013. From top to bottom, the images were taken at 22:48:22, 22:49:59, 22:51:32 and 22:53:07 GMT. (courtesy: ESA)

The low-resolution camera was originally installed on Mars Express for visual confirmation that the Beagle-2 lander had separated in 2003. In 2007 it was switched back on and used primarily for outreach, education and citizen science, with images automatically posted to a dedicated Flickr page, sometimes within just 75 minutes of being taken at Mars.

Last year, with new software, the camera was adopted as a supporting science instrument. Now, the first paper has been published, on detached, high-altitude cloud features and dust storms over the edge, or ‘limb’, of the planet.

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Example of a cloud event captured by ESA’s Mars Express Visual Monitoring Camera on 15 December 2009 over the equator. The cloud formation reaches a maximum altitude of 40 km and spans 830 km horizontally. It shows interesting features such as the ‘blobs’, which include a detached tilted element in the north–south direction, suggesting that it is shaped by the action of meridional winds. The event occurred close to the spring equinox for the northern hemisphere suggesting it is a condensate cloud of water-ice particles. From top to bottom, the images were taken on 15 December 2009 at 06:48:41, 06:49:25, 06:50:51, 06:51:35 and 06:52:19 GMT. (courtesy: ESA)

While these limb clouds can be imaged by other instruments or spacecraft, it is not necessarily their main task – they are usually looking directly at the surface with a narrow field of view that covers a small portion of the planet for specialised study. By contrast, the webcam often has a global view of the full limb.

“For this reason, limb observations in general are not so numerous, and this is why our images are so valuable in contributing to our understanding of atmospheric phenomena,” says Agustin Sánchez-Lavega, lead author of the study from the University del Pais Vasco in Bilbao, Spain.

“Combining with models and other datasets we were able to gain a better insight to understanding atmospheric transport and seasonal variations that play a role in generating the high-altitude cloud features.”

The catalogue of some 21 000 images taken between 2007 and 2016 were examined and 300 identified for the study.

Multiple images separated by a few minutes each were obtained for 18 events as they rotated into view, providing visual documentation of the features from different perspectives.

In general, the cloud features imaged by the camera have peak altitudes in the range of 50–80 km above the planet and extend horizontally from about 400 km up to 1500 km.

In order to understand the nature of the clouds – for example, if they were primarily composed of dust or icy particles – the team compared the images with atmospheric property predictions detailed by the Mars Climate Database. The database uses temperature and pressure information to indicate if either water or carbon dioxide clouds could be capable of forming at that time and altitude.

The team also looked at the weather report generated from images by NASA’s Mars Reconnaissance Orbiter, and in some cases had additional corresponding observations obtained from other sensors on ESA’s Mars Express.

From the 18 studied in depth, most were concluded to be water-ice clouds, and one was attributed to a dust storm.

The high water-ice clouds seemed to depend on the position of the sun: they are present at sunrise and early afternoon, when temperatures are lower, allowing water-ice to condense. Later in the day, as the sunlight increases, the water-ice evaporates, and they dissipate.

Temperature variability and water vapour content according to the season, as well as atmospheric dynamics, can also play a role in the visible characteristics of the clouds.

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Example of dust clouds imaged by ESA’s Mars Express Visual Monitoring Camera and NASA’s Mars Reconnaissance Orbiter’s Mars Colour Imager (MARCI) in November 2007 over the Utopia region. Arrows indicate the dust front in each image. For the MARCI image (top left) and the VMC image at bottom right, a recognisable surface feature is marked on the image, aiding identification of the dust front in both images. The arced dust front had a length of 730 km on its internal edge and 1950 km on its outer arc, and a width of about 60–130 km. Limb observations by VMC indicated the altitude was about 65 km. (courtesy: MARCI: NASA/JPL/MSSS; VMC: ESA)

One event was attributed to a local dust storm in the northern hemisphere, which was also captured by images taken looking down on the surface by the Mars Reconnaissance Orbiter. The storm evolved rapidly, and took on arc shape with a front of about 1950 km on its outer edge and 730 km on its internal edge, and a width of 60–130 km. Limb observations by the webcam indicated the altitude was about 65 km.

“This long-term monitoring has allowed us to detect and measure the extent of dust and clouds over the limb of the planet, and study changes with a high cadence of imaging,” says Dmitri Titov, ESA’s Mars Express project scientist.

“We will continue to maintain the database with systematic observations from the webcam to provide wide views of atmospheric phenomena.”