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High-Resolution Stereo Camera (HRSC) nadir and colour channel data taken
during revolution 10743 on 8 June 2012 by ESA’s Mars Express have been
combined to form a natural-colour view of Hooke Crater region in Argyre.
Centred at around 45°S and 314°E, this image has a ground resolution of
about 22 m per pixel. The image shows the western half of the 138
km-wide Hooke Crater, with wind formed dunes at its heart, while to the
left of the crater, the ice-covered plains of Argyre Planitia are coated
with a thin dusting of frozen carbon dioxide. The very large Argyre
impact basin brought materials from the deeper martian crust and mantle
to the surface. It provides scientists with one of the locations on Mars
with a greater mixture of young/old and deep/surface terrains,
providing a window into the planet’s past.
Credits: ESA/DLR/FU Berlin (G. Neukum)
On 8 June, the high-resolution stereo camera on Mars Express captured a
region within the 1800 km-wide and 5 km-deep Argyre basin, which was
created by a gigantic impact in the planet’s early history.
After Hellas, the Argyre impact basin is the second largest on the Red Planet.
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This computer-generated perspective view was created using data obtained
from the High-Resolution Stereo Camera (HRSC) on ESA’s Mars Express.
Centred at around 45°S and 314°E, this image has a ground resolution of
about 22 m per pixel. The lower right of the image shows the wind-formed
dunes within Hooke Crater, while small deposits of frozen carbon
dioxide ice lie within the crater, the top left of the image starts to
show the more extensive ice lying on the surrounding Argyre Planitia.
Credits: ESA/DLR/FU Berlin (G. Neukum)
The name stems from the Greek word ‘argyros’ (silver) and Argyre was an
‘island of silver’ in Greek and Roman mythology. Giovanni Schiaparelli,
the famed Italian astronomer, gave the name to this bright region on
Mars in his detailed 1877 map.
At the centre of the larger impact basin is a flat region known as
Argyre Planitia. The Mars Express images in this release all show a
portion of the northern part of this plain, with a large portion of each
image dominated by the western half of the 138 km-wide Hooke Crater,
named after the British physicist and astronomer Robert Hooke.
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Hooke Crater and the surrounding Argyre Planitia are seen in broader
context. The smaller rectangle shows the region covered in this ESA Mars
Express HRSC image release.
Credits: NASA MGS MOLA Science Team
Most of Argyre Planitia has been shaped by wind, glacial and
lacustrine (lake-based) processes, creating the smoother appearance of
the landscape surrounding Hooke Crater.
Inside Hooke Crater itself, prevailing wind activity has formed dunes
and helped to create linear erosion features, clearly seen in the
following topographic image.
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This colour-coded plan view is based on a digital terrain model of the
region, from which the topography of the landscape can be derived. The
colour coding highlights the difference between the elevation of the
hills to the right of the image and the depth of the Argyre Planitia
region as well as Hooke Crater itself. This topographic map also
increases the visibility and contrast of the dune features within Hooke
Crater. Centred at around 45°S and 314°E, the image has a ground
resolution of about 22 m per pixel.
Credits: ESA/DLR/FU Berlin (G. Neukum)
The most striking feature of this image release, shown clearly in the
first image at the top of the page, is the icing sugar-like covering of
the surface to the south (left) of the image. This is frost, but made of
carbon dioxide, not water.
Carbon dioxide ice is commonly seen on the surface of Mars, and has long
been thought to form only at ground level, freezing out of the
atmosphere as frost, which is most likely the case here.
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Argyre Planitia and Hooke Crater imaged during revolution 10743 on 8
June 2012 by ESA’s Mars Express using the High-Resolution Stereo Camera
(HRSC). Data from HRSC’s nadir channel and one stereo channel are
combined to produce this anaglyph 3D image that can be viewed using
stereoscopic glasses with red–green or red–blue filters. Centred at
around 45°S and 314°E, the image has a ground resolution of about 22 m
per pixel.
Credits: ESA/DLR/FU Berlin (G. Neukum)
The lowlands to the south (left in the first image) of Hooke and regions
within the crater are covered by a thin ice layer. However, it is
lacking on the inner north-facing crater wall. It was probably melted
there by the Sun, as indicated by the timing of the image.
Taken at around 4:30 in the local afternoon and during the southern
hemisphere’s mid-winter, the Sun would have been just over 20 degrees
above the horizon. It should then have been able to melt ice on the
steeper north-facing slopes, but would probably not have had enough time
to warm and melt any on low-lying horizontal surfaces.
Schiaparelli would doubtless have marvelled at the exquisite images
coming back from Mars Express, which continues to provide today’s
scientists with a bounty of wonderful data.
ESA
Guillermo Gonzalo Sánchez Achutegui
ayabaca@gmail.com
ayabaca@hotmail.com
ayabaca@yahoo.com
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High-Resolution
Stereo Camera (HRSC) nadir and colour channel data taken during
revolution 10572 on 9 April 2012 by ESA’s Mars Express have been
combined to form a natural-colour view of Hadley Crater. Centred at
around 19°S and 157°E, the image has a ground resolution of about 19 m
per pixel. The image shows the main 120 km wide crater, with subsequent
impacts at later epochs within it. Evidence of these subsequent impacts
occurring over large timescales is shown by some of the craters being
buried. 
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