jeudi 19 février 2015

Mars hills hide icy past












ESA - Mars Express Mission patch.

19 February 2015

Phlegra Montes southern tip

A complex network of isolated hills, ridges and small basins spanning 1400 km on Mars is thought to hide large quantities of water-ice.

Phlegra Montes stretches from the Elysium volcanic region at about 30ºN and deep into the northern lowlands at about 50°N, and is a product of ancient tectonic forces. Its age is estimated to be 3.65–3.91 billion years.

ESA’s Mars Express imaged the portion of Phlegra Montes seen here on 8 October 2014. It captures the southernmost tip of the range centred on 31ºN / 160ºE.

Phlegra Montes in context

Based on radar data from NASA’s Mars Reconnaissance Orbiter combined with studies of the region’s geology from other orbiters, scientists believe that extensive glaciers covered this region several hundred million years ago.

And it is thought that ice is still there today, perhaps only 20 m below the surface.

The tilt of the planet’s polar axis is believed to have varied considerably over time, leading to significantly changing climatic conditions. This allowed the development of glaciers at what are today the mid-latitudes of Mars.

Phlegra Montes southern tip topography

Features visible in the Phlegra Montes mountain range providing strong evidence for glacial activity include aprons of rocky debris surrounding many of the hills. Similar features are seen in glacial regions on Earth, where material has gradually slumped downhill through the presence of subsurface ice.

Additional features in the region include small valleys cutting through the hills and appearing to flow into regions of lower elevation, in particular towards the centre of the image.

Perspective view of Phlegra Montes

The hummocky terrain provides a distinct contrast to the smooth plains that dominate the upper portion of this image. The material here is thought to be volcanic in origin, perhaps originating from the Hecates Tholus volcano in Elysium some 450 km to the west, some time after the formation of Phlegra Montes.

Upon closer inspection, ‘wrinkle ridges’ can be seen in the lava plain. These features arise from the cooling and contraction of lava owing to compressive tectonic forces following its eruption onto the surface.

Phlegra Montes southern tip in 3D

This region of Phlegra Montes and its local surrounds illustrate some of the key geological processes that have worked to shape the Red Planet over time, from ancient tectonic forces, to glaciation and volcanic activity.

More about...:

Looking at Mars: http://www.esa.int/Our_Activities/Space_Science/Mars_Express

Mars Express overview: http://www.esa.int/Our_Activities/Space_Science/Mars_Express_overview

Mars Express 10 year brochure: http://esamultimedia.esa.int/multimedia/publications/BR-312/

Related links:

High Resolution Stereo Camera: http://berlinadmin.dlr.de/Missions/express/indexeng.shtml

Behind the lens...: http://www.esa.int/Our_Activities/Space_Science/Mars_Express/Behind_the_lens

Frequently asked questions: http://www.esa.int/Our_Activities/Space_Science/Mars_Express/Frequently_asked_questions

ESA Planetary Science archive (PSA): http://www.rssd.esa.int/PSA

NASA Planetary Data System: http://pds-geosciences.wustl.edu/missions/mars_express/hrsc.htm

HRSC data viewer: http://hrscview.fu-berlin.de/

In depth:

Mars Express in depth: http://sci.esa.int/science-e/www/area/index.cfm?fareaid=9

Mars Express top 10 discoveries: http://sci.esa.int/jump.cfm?oid=51820

Mars Express blog: http://blogs.esa.int/mex/

Mars Webcam: http://blogs.esa.int/vmc

Images, Text, Credits: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO/NASA MGS MOLA Science Team.

Best regards, Orbiter.ch

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