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Mars Exploration by Orbit Copyright © 2004 The McGraw-Hill Companies The European Space Agency's (ESA) first mission to Mars, called Mars Express, was launched June2, 2003 and entered an orbit around the planet by December 25. This Image Gallery exhibits a number of images of Mars captured by the High Resolution Stereo Camera (HRSC), OMEGA, and PFS (Planetary Fourier Spectrometer) onboard Mars Express. Text by Jo Turner Images Courtesy of the European Space Agency Title page image courtesy of ESA/DLR/FU Berlin (G. Neukum)

1. Марс Express приближение (Image: ESA/DLR/FU Berlin (G. Neukum)) This picture was taken on December 1, 2003, from the European Space Agency's Mars Express spacecraft by the High Resolution Stereo Camera (HRSC). It shows planet Mars as seen from a distance of about 5.5 million kilometers (3.4 million miles). Due to the location of the spacecraft, the illumination of the planet is shown in a way that could never be seen from Earth. The Sun shines on part of the western hemisphere, while more than a third of the planet lies in darkness. The dark features at the top are part of the northern lowlands of Mars, where oceans may have existed thousands of millions of years ago.

2. Топография Марса (Image: NASA/MGS) Two hemispheres of Mars are shown in this image, released on May 27, 1999, and taken by the Mars Orbiter Laser Altimeter (MOLA), an instrument onboard NASAs Mars Global Surveyor. In the first image, the most prominent feature is the massive Hellas impact basin (upper left) in the southern hemisphere, which is nearly 10 km (6 mi) deep and 2000 km (1200 mi) across. The lower right image shows the Tharsis province containing the Tharsis mountains (Ascraeus, Pavonis, and Arsia), and the Valles Marineris canyon system and related outflow channels. The most striking aspect of the topographic map is the difference between the planets low, smooth northern hemisphere and the heavily cratered southern hemisphere.

3.Цветное фото кратера Гусева (Image: ESA/DLR/FU Berlin (G. Neukum)) This color picture was taken by the High Resolution Stereo Camera (HRSC) camera from an altitude of 320 km (199 mi) on January 16, It shows the center of Gusev crater where the NASA Spirit rover landed. Gusev is a crater 160 km (100 mi) in diameter. Earlier in the history of Mars, it appears that this area was covered by water. The area shown measures about 60 km (37 mi) across at the bottom. North is at the top. Many craters on Mars, especially at latitudes greater than 45°, are surrounded by lobed patterns (the round shapes below the dark areas in this picture), which suggests that the impacting object struck wet or icy ground. By looking at the size of craters surrounded by lobate flows, scientists are able to estimate the depth of the ice table beneath the ground. The MARSIS experiment on-board the Mars Express orbiter will sound for underground water.

4. Hecates Tholus volcano (Image: ESA/DLR/FU Berlin (G. Neukum)) This color image of the Hecates Tholus volcano was taken by the High Resolution Stereo Camera (HRSC) on Mars Express in orbit 32 from an altitude of 275 km (171 mi) on March 1, It shows the summit caldera of Hecates Tholus, the northernmost volcano of the Elysium volcano group. The image center is located at 150°E and 31.7°N. North is at the top. The volcano has an elevation of 5300 m (17,400 ft), and the caldera has a maximum diameter of 10 km (6 mi) and a depth of 600 m (2000 ft). The volcano reveals multiple caldera collapses. On the flanks of Hecates Tholus several flow features related to water (lines radiating outward) and pit chains related to lava can be observed.

5. HRSC color image of Louros Valles (Image: ESA/DLR/FU Berlin (G. Neukum)) This image was taken by the High Resolution Stereo Camera (HRSC) during orbit 97 from an altitude of 269 km (167 mi) on April 8, The image has a resolution of about 13 m (43 ft) per pixel and is centered at °E and 8.3°S. The color image was created from the nadir (the vertical view) and three color channels. North is at the right. The image shows a system of sapping channels (where the surface is eroded by water coming from a source below) called Louros Valles (named in 1982 after a river in Greece), south of the Ius Chasma canyon which runs west to east. The Ius Chasma belongs to the giant Valles Marineris canyon system. The Geryon Montes, visible at the northern border, is a mountain range which divides the Ius Chasma into two parallel trenches. The dark deposits at the bottom of the Ius Chasma could be related to water and wind erosion, as similar phenomena are observed on Earth.

6. Perspective view of Acheron Fossae (Image: ESA/DLR/FU Berlin (G. Neukum)) These images, taken May 7, 2004, by the High Resolution Stereo Camera (HRSC), are of the Acheron Fossae region, an area of intensive tectonic activity in the past. The images show traces of enormous stress and corresponding strain in the crust of the Red Planet. The HRSC was pointed twice at this interesting geological feature during orbits 37 and 143. The feature is situated at approximately °N and °E, about 1000 km (600 mi) north of the large Olympus Mons volcano. This perspective view shows the region plus some adjacent areas to the south without vertical exaggeration. This view is dominated by the curved faults, showing a highly fractured and deformed area in the central part of the Acheron Fossae. In geological terms, this is called a horst and graben system. When several parallel faults form, the block of crust between them drops down, forming a graben. At Acheron, an example of parallel fault-bounded grabens has formed, dissected by remnants of the preexisting topographical heights, the horsts.

7. Perspective view of flank of Olympus Mons (Image: ESA/DLR/FU Berlin (G. Neukum)) This image, with a resolution of about 25 ms (80 ft) per pixel and centered at 222°E and 22°N, was taken by the High Resolution Stereo Camera (HRSC) during orbit 143 from an altitude of 266 km (165 mi) on April 21, North is to the left. The image shows the western flank of the shield volcano Olympus Mons in the Tharsis region of the Martian western hemisphere. The escarpment rises from the surface level to over 7000 m (23,000 ft). The lower part of the image shows the start of the extensive plains west of the escarpment, known as the 'aureole'. To the north and west of the volcano, these aureole deposits are regions of gigantic ridges and blocks extending 1000 (600 mi) from the summit. These were possibly caused by landslides. Large masses of shield material can be found in the aureole area. Indications such as sediment distribution also suggest a development and resurfacing connected to glacial activity.

8. Southern part of Olympus Mons caldera (Image: ESA/DLR/FU Berlin (G. Neukum)) This perspective view shows the southern part of the caldera (summit crater) of the Olympus Mons volcano on Mars. The image has been calculated from the digital elevation model derived from the stereo channels and combined with the nadir and color channels of the High Resolution Stereo Camera (HRSC). The data were retrieved from a height of 273 km (170 mi) in orbit 37 on January 21, The view is centered at 18.3°N and 227°E. The image is about 40 km (25 mi) across. The vertical exaggeration is 1.8 arcsec. South is up.

9. Reull Vallis HRSC image (Image: ESA/DLR/FU Berlin (G. Neukum)) This picture was taken by the High Resolution Stereo Camera (HRSC) during orbit 18 on January 15, 2004, from a height of 273 km (170 mi). The location is east of the Hellas basin at 41°S and 101°E. The area is 100 km (60 mi) across, resolution of 12 m (40 ft) per pixel, and shows a channel (Reull Vallis) is seen that could have been formed by flowing water. The landscape is seen in a perspective view, with North at the top.

12. OMEGA view of Martian south pole (Image: ESA-OMEGA) This map, released on March 17, 2004, of the Martian south pole was derived from infrared spectral images acquired by OMEGA, showing the bright polar cap, rich in carbon dioxide (light pink), surrounded by water- rich ice, free of carbon dioxide (green to blue). OMEGA will determine mineral composition from the visible and infrared light reflected from the planets surface in the wavelength range micrometers. As light reflected from the surface must pass through the atmosphere before entering the instrument, OMEGA will also measure aspects of atmospheric composition.

13. OMEGA image of southern polar cap (Image: ESA-OMEGA) OMEGA observed the southern polar cap of Mars on January 18, 2004, as seen on all three bands. The right one represents the visible image, the middle one the CO 2 (carbon dioxide) ice, and the left one the H 2 O (water) ice.

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