Hi My Friends: A VUELO DE UN QUINDE EL BLOG., ESA’s Mars Express has imaged an area to the south of the famed Valles
Marineris canyon on the Red Planet, showing a wide range of tectonic and
impact features.
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High-Resolution Stereo Camera (HRSC) nadir and colour channel data taken
during revolution 10532 on 17 April 2012 by ESA’s Mars Express have
been combined to form a natural-colour view of the Melas Dorsa region.
Centred at around 18°S and 288°E, this image has a ground resolution of
about 18 m per pixel. The image shows the wrinkle ridges bisected by
crustal displacement faults known as ‘en-echelon’ faults along with the
large impact crater with its butterfly-shaped fluidised ejecta blanket.
En-echelon faults are closely spaced, parallel overlapping or step-like
fault structures, which in this view can be seen at the far left of the
image, intersecting the wrinkle ridges.
ESA’s Mars Express has imaged an area to the south of the famed Valles
Marineris canyon on the Red Planet, showing a wide range of tectonic and
impact features.
On 17 April, the orbiter pointed its high-resolution stereo camera at the Melas Dorsa region of Mars. This area sits in the volcanic highlands of Mars between Sinai and Thaumasia Plana, 250 km south of Melas Chasma. Melas Chasma itself is part of the Valles Marineris rift system. The image captures wrinkle ridges, some unusual intersecting faults and an elliptical crater surrounded by ejecta in the shape of a butterfly and with a strange ‘fluid-like’ appearance.
On 17 April, the orbiter pointed its high-resolution stereo camera at the Melas Dorsa region of Mars. This area sits in the volcanic highlands of Mars between Sinai and Thaumasia Plana, 250 km south of Melas Chasma. Melas Chasma itself is part of the Valles Marineris rift system. The image captures wrinkle ridges, some unusual intersecting faults and an elliptical crater surrounded by ejecta in the shape of a butterfly and with a strange ‘fluid-like’ appearance.
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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 18°S and 288°E, this image has a ground resolution of
about 18 m per pixel. The 16 km-wide impact crater and its associated
butterfly-shaped ejecta blanket takes up most of this image. The shape
of the crater and ejecta blanket indicates a low-angle impact by a comet
or asteroid.
Credits: ESA/DLR/FU Berlin (G. Neukum)
Melas Dorsa impact crater perspective view
Elliptical craters like this 16 km-wide example are formed when asteroids or comets strike the surface of the planet at a shallow angle. Scientists have suggested that a fluidised ejecta pattern indicates the presence of subsurface ice which melted during the impact. Subsequent impacts have created a number of smaller craters in the ejecta blanket.
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| Zoom view of the flooded crater seen in the upper centre part of the main image. | Credits: ESA/DLR/FU Berlin (G. Neukum) | |
| The rim of another large crater is visible in the upper centre part
of the image, but it appears mostly to have been almost buried during
some distant epoch by volcanic dust and ash.
This makes any detailed study of it almost impossible. However, its centre shows concentric deposits that could provide insights into the composition of the volcanic material that buried it. | ||
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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. Notable here is the almost complete lack of relief change in
the crater at the top of the image, which has been filled in by volcanic
activity. Centred at around 18°S and 288°E, the image has a ground
resolution of about 18 m per pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
Melas Dorsa topography
Several wrinkle ridges can be seen across the image. These form when horizontal compression forces in the crust pushes the crust upwards. To the left, the ridges are bisected by crustal displacement faults. These have cut into the ridges and the surrounding surface at some later epoch. This highlights the different tectonic phases responsible the formation of this region.
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Melas Dorsa is seen here in broader context. The smaller rectangle shows
the region covered in this ESA Mars Express HRSC image release. Melas
Dorsa is located in the volcanic highlands of Mars between Sinai and
Thaumasia Plana, approximately 250 km south of Melas Chasma. Melas
Chasma itself belongs to the Valles Marineris rift system.
Credits: NASA MGS MOLA Science Team
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Melas Dorsa imaged during revolution 10532 on 17 April 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. The image clearly shows the wrinkle
ridges bisected by the en echelon fault lines. Centred at around 18°S
and 288°E, the image has a ground resolution of about 18 m per pixel.
Credits: ESA/DLR/FU Berlin (G. Neukum)
Credits: ESA/DLR/FU Berlin (G. Neukum)
ESA
Guillermo Gonzao Sánchez Achuteguiayabaca@gmail.com
ayabaca@hotamil.com
ayabaca@yahoo.com
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