http://www.cieletespacephotos.fr/main.php L'IMAGE DU JOUR : La nébuleuse du Pelican (IC 5067) avec des objets HH par Ken Crawford ... ->
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ROBONAUT 2, le premier androïde spatial !
R2 vient d'arriver au centre spatial Kennedy. Il partira avec la prochaine navette Discovery (STS-133) pour rejoindre l'ISS. Sa mission aider les astronautes à exécuter des travaux de maintenance répétitifs ou risqués.
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Bonne visite, bonne recherche !]]> en-us Ciel et Espace Photos Gallery 2 RSS Module, version 1.1.0 Thu, 09 Sep 2010 03:07:41 +0200 240 http://www.cieletespacephotos.fr/main.php?g2_view=core.DownloadItem&g2_itemId=50454 http://www.cieletespacephotos.fr/main.php http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-03high.jpg.html
Observation du ciel par un amateur avec son telescope. Juillet 2010
Dans l'album L'OBSERVATION : les Nuits des Etoiles, les constellations, les spectacles astro,...]]> photo Wed, 08 Sep 2010 12:18:45 +0200 http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-02high.jpg.html
Observation du ciel par un amateur avec son telescope. Juillet 2010
Dans l'album L'OBSERVATION : les Nuits des Etoiles, les constellations, les spectacles astro,...]]> photo Wed, 08 Sep 2010 12:18:45 +0200 http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Observation/850-02075-01high.jpg.html
Observation du ciel par un amateur avec son telescope. Juillet 2010
Dans l'album L'OBSERVATION : les Nuits des Etoiles, les constellations, les spectacles astro,...]]> photo Wed, 08 Sep 2010 12:18:45 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/020-00320-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/020-00320-03high.jpg.html
ESO has released a spectacular new image of NGC 300, a spiral galaxy similar to the Milky Way, and located in the nearby Sculptor Group of galaxies. Taken with the Wide Field Imager (WFI) at ESO’s La Silla Observatory in Chile, this 50-hour exposure reveals the structure of the galaxy in exquisite detail. NGC 300 lies about six million light-years away and appears to be about two thirds the size of the full Moon on the sky.
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Wed, 08 Sep 2010 12:18:21 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/Galaxies/020-00320-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/Galaxies/020-00320-03high.jpg.html
ESO has released a spectacular new image of NGC 300, a spiral galaxy similar to the Milky Way, and located in the nearby Sculptor Group of galaxies. Taken with the Wide Field Imager (WFI) at ESO’s La Silla Observatory in Chile, this 50-hour exposure reveals the structure of the galaxy in exquisite detail. NGC 300 lies about six million light-years away and appears to be about two thirds the size of the full Moon on the sky.
Dans l'album Les galaxies]]> photo Wed, 08 Sep 2010 12:18:06 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/017-02301-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/017-02301-03high.jpg.html
The IC 5067 nebula (Pelican Nebula) with HH Objects
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Wed, 08 Sep 2010 09:46:13 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/Nebuleuses/017-02301-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/Nebuleuses/017-02301-03high.jpg.html
The IC 5067 nebula (Pelican Nebula) with HH Objects
Dans l'album Les nébuleuses]]> photo Wed, 08 Sep 2010 09:45:56 +0200 http://www.cieletespacephotos.fr/main.php/v/Observation/Conjonction/026-02920-11high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Observation/Conjonction/026-02920-11high.jpg.html
Conjonction entre la Lune et l'amas ouvert de la Creche (M44). Conjonction between Moon and M44 open cluster. 06/09/10
Dans l'album Les conjonctions]]> photo Tue, 07 Sep 2010 14:48:50 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/028-00150-07high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/028-00150-07high.jpg.html
Passage du satellite Metop sur fond de voie lactee.
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Tue, 07 Sep 2010 14:48:25 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/VoieLactee/028-00150-07high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/VoieLactee/028-00150-07high.jpg.html
Passage du satellite Metop sur fond de voie lactee.
Dans l'album La voie lactée]]> photo Tue, 07 Sep 2010 14:48:12 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/AmasOuverts/019-01202-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/AmasOuverts/019-01202-03high.jpg.html
L'amas ouvert NGC 6791 dans la constellation de la Lyre. NGC 6791 open cluster in Lyra Constellation
Dans l'album Les amas ouverts]]> photo Tue, 07 Sep 2010 14:47:52 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/017-04360-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/017-04360-01high.jpg.html
Nebuleuse IC 5076 (spot bleu) dans la constellation du Cygnus. IC 5076 nebula (Blue Spot) in Cygnus constellation
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Tue, 07 Sep 2010 14:47:29 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/Nebuleuses/017-04360-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/Nebuleuses/017-04360-01high.jpg.html
Nebuleuse IC 5076 (spot bleu) dans la constellation du Cygnus. IC 5076 nebula (Blue Spot) in Cygnus constellation
Dans l'album Les nébuleuses]]> photo Tue, 07 Sep 2010 14:47:17 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03292-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03292-02high.jpg.html
Mars digital-image mosaic merged with color of the MC-23 quadrangle, Aeolis region of Mars. The southern part is dominated by heavily cratered highlands that are cut by two large channels having features characteristic of terrestrial river beds. The highlands are separated from the northern plains of Elysium Planitia by a highly dissected, discontinuous northwest trending scarp. The northeastern part is marked by a large shield volcano, Apollinaris Patera. Latitude range - 30 to 0 degrees, longitude range -180 to -135 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03292-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03292-01high.jpg.html
Mars digital-image mosaic merged with color of the MC-22 quadrangle, Mare Tyrrhenum region of Mars. Heavily cratered highlands dominate the Mare Tyrrhenum quadrangle. The central part is marked by a large shield volcano, Tyrrhena Patera, and associated ridged plains of Hesperia Planum that probably are made up of basaltic lava flows. Latitude range -30 to 0 degrees, longitude range -135 to -90 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-04high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-04high.jpg.html
Mars digital-image mosaic merged with color of the MC-21 quadrangle, Iapygia region of Mars. Heavily cratered and in places dissected highlands dominate the Iapygia quadrangle. The west-central part is marked by a large impact crater, Huygens. Huygens is an ancient remnant of the many large impact events that occurred during the period of heavy bombardment. The southern one-third is characterized by mountainous and knobby terrain of the northern rim of the enormous Hellas impact basin. Latitude range -30 to 0 degrees, longitude range -90 to -45 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-03high.jpg.html
Mars digital-image mosaic merged with color of the MC-20 quadrangle, Sinus Sabeus region of Mars. Heavily cratered highlands dominate the Sinus Sabeus quadrangle. The northern part is marked by a large impact crater, Schiaparelli. Schiaparelli is an ancient remnant of the many large impact events that occurred during the period of heavy bombardment. Latitude range -30 to 0 degrees, longitude range -45 to 0.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-02high.jpg.html
Mars digital-image mosaic merged with color of the MC-19 quadrangle, Margaritifer Sinus region of Mars. Heavily cratered highlands, which dominate the Margaritifer Sinus quadrangle, are marked by large expanses of chaotic terrain. In the northwestern part, the major rift zone of Valles Marineris connects with a broad canyon filled with chaotic terrain. Latitude range -30 to 0, longitude range 0 to 45 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03290-01high.jpg.html
Mars digital-image mosaic merged with color of the MC-18 quadrangle, Coprates region of Mars. Moderately cratered and faulted highland ridged plains in the northern and southern parts are cut by the prominent Valles Marineris chasma system, which reaches depths of 10 km and extends in an east-southeast direction for about 2,500 km across the quadrangle. The long, central canyons appear to be large, fault-bounded rifts, whereas some of the isolated, northern canyons are the sources of large outflow channels. Latitude range -30 to 0 degrees, longitude range 45 to 90 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-07high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-07high.jpg.html
A color image of the Tharsis region of Mars; north toward top. The scene shows the Tharsis bulge, a huge ridge covered by the 3 large aligned Tharsis Montes shield volcanoes (from lower left to right): Arsia, Pavonis, and Ascraeus Mons. To the left of the Tharsis Montes lies the huge Olympus Mons shield volcano, followed clockwise by Alba Patera (north center), several smaller volcanoes, and the linear depressions of Mareotis and Tempe Fossae (upper right). This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 50 degrees N. to 20 degrees S. and from longitude 85 degrees to 150 degrees. Mercator projection is used between latitudes 20 degrees S. and 30 degrees N.; Lambert projection is used above latitude 30 degrees N. The Tharsis bulge encompasses the most intensely and most recently active volcanic region of the planet. Each Tharsis Montes volcano is 350-400 km in diameter and about 17 km above the surrounding plain. The volcanoes are about 700 km apart and appear to be above a major northeast-trending fracture zone along the bulge, now buried by volcanic deposits. Olympus Mons (left center) is the largest known volcano in the Solar System. It is 27 km high, over 600 km at the base, and is surrounded by a well-defined scarp that is up to 6 km high. The summit calderas (central depressions) of all four volcanoes probably formed from recurrent collapse following drainage of magma resulting from flank eruptions. 1,600-km-diameter Alba Patera (north center) far exceeds any other known volcano in areal extent; it covers eight times the area of Olympus Mons but reaches only about 6 km in height. Fossae (linear depressions) of the Tharsis area are fault-bound graben formed by upwarping of the Tharsis bulge.

Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-06high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-06high.jpg.html
A color image of the south Chryse basin Valles Marineris outflow channels on Mars; north toward top. The scene shows on the southwest corner the chaotic terrain of the east part of Valles Marineris and two of its related canyons: Eos and Capri Chasmata (south to north). Ganges Chasma lies directly north. The chaos in the southern part of the image gives rise to several outflow channels, Shalbatana, Simud, Tiu, and Ares Valles (left to right), that drained north into the Chryse basin. The mouth of Ares Valles is the site of the Mars Pathfinder lander. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 20 degrees S. to 20 degrees N. and from longitude 15 degrees to 53 degrees; Mercator projection. The south Chryse outflow channels are cut an average of 1 km into the cratered highland terrain. This terrain is about 9 km above datum near Valles Marineris and steadily decreases in elevation to 1 km below datum in the Chryse basin. Shalbatana is relatively narrow (10 km wide) but can reach 3 km in depth. The channel begins at a 2- to 3-km-deep circular depression within a large impact crater, whose floor is partly covered by a chaotic material, and ends in Simud Valles. Tiu and Simud Valles consist of a complex of connected channel floors and chaotic terrain and extend as far south as and connect to eastern Valles Marineris. Ares Vallis originates from discontinuous patches of chaotic terrain within large craters. In the Chryse basin the Ares channel forks; one branch continues northwest into central Chryse Planitia (Latin for plain) and the other extends north into eastern Chryse Planitia.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-05high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-05high.jpg.html
A color image of the Hellas Planitia region of Mars; north toward top. The scene shows the Hellas plain within the 1,800- km-diameter Hellas basin, an ancient impact basin (and the largest basin on Mars) formed when a large projectile (asteroid, comet, meteor) hit the surface. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 60 degrees S. to 20 degrees S. and from longitude 250 degrees to 320 degrees. Mercator projection is used between latitudes 20 degrees S. and 30 degrees S.; Lambert projection is used below latitude 30 degrees S. The exact diameter of the ancient Hellas basin is difficult to determine because large portions of the rim are missing to the northeast and southwest. In addition several large patera or low volcanoes (Tyrrhena, Hadriaca, Amphitrites) occur along or near the rim and their flows have partially buried the older impact deposits. Outside the rim are several large, arcuate, inward-facing escarpments which could be remnants of multiple rings. The plains of Hellas are very complex; fluvial channels drain into the basin and the plains have been described as being a mixture of fluvial, lacustrine, glacial, eolian, and volcanic deposits. Frequent dust storms occur within the basin.

Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-04high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-04high.jpg.html
Mars digital-image mosaic merged with color of the MC-17 quadrangle, Phoenicis Lacus region of Mars. Two of the four largest shield volcanoes on Mars are within the northwestern part, the south half of Pavonis Mons and Arsia Mons. The eastern part includes Syria and Sinai Plana. Most of the quadrangle forms the Tharsis plateau--the highest plateau on Mars; its elevation, 10 km, is twice that of the Tibetan Plateau, the highest plateau on Earth. Also in the northeastern part is Noctis Labyrinthus, a complex system of fault valleys at the west end of Valles Marineris. The south-central part is marked by the large fault system, Claritas Fossae. Latitude range -30 to 0 degrees, longitude range 90 to 135 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-03high.jpg.html
Mars digital-image mosaic merged with color of the MC-16 quadrangle, Memnonia region of Mars. Heavily cratered highlands in the southern two-thirds are cut in the northeastern part by a large outflow channel, Mangala Vallis. The highlands are bounded to the north by undulating wind-eroded deposits and to the east by lava flows of the Tharsis region. Latitude range -30 to 0 degrees, longitude range 135 to 180 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-02high.jpg.html
Mars digital-image mosaic merged with color of the MC-15 quadrangle, Elysium region of Mars. The Elysium quadrangle includes relatively smooth lowland plains immediately north of the more cratered highlands. The plains are interrupted on the northwest by two large shield volcanoes, Elysium Mons and Albor Tholus. The plains are also marked by an elongate crater, Orcus Patera, at the east boundary and a band of knobby terrain that extends northeastward through the eastern part. Latitude range 0 to 30 degrees, longitude range -180 to -135 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03288-01high.jpg.html
Mars digital-image mosaic merged with color of the MC-14 quadrangle, Amenthes region of Mars. The southern part includes heavily cratered highlands. The northern part is dominated by relatively smooth plains of Elysium Planitia and the eastern half of the Isidis basin. Latitude range 0 to 30 degrees, longitude range -135 to -90 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-04high_001.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-04high_001.jpg.html
Mars digital-image mosaic merged with color of the MC-13 quadrangle, Syrtis Major region of Mars. The central part is dominated by dark dust and lava flows of the Syrtis Major Planitia region. These lava flows are partly bounded to the east by a large depression, Isidis basin, which contains smooth plains, and to the west and north by heavily cratered and moderately faulted highlands. Latitude range 0 to 30 degrees, longitude range -90 to -45 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-03high.jpg.html
Mars digital-image mosaic merged with color of the MC-12 quadrangle, Arabia region of Mars. Heavily cratered highlands dominate the Arabia quadrangle. The northeastern part is marked by a large impact crater, Cassini. Cassini is an ancient remnant of the many large impact events that occurred during the period of heavy bombardment. Latitude range 0 to 30 degrees, longitude range -45 to 0 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-02high.jpg.html
Mars digital-image mosaic merged with color of the MC-11 quadrangle, Oxia Palus region of Mars. Heavily cratered highlands of the southeastern two-thirds are cut by several large outflow channels. These channels terminate at the dark large depression, Chryse basin, which contain relatively smooth plains in the northwestern part. Latitude range 0 to 30 degrees, longitude range 0 to 45 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03286-01high.jpg.html
Mars digital-image mosaic merged with color of the MC-10 quadrangle, Lanae Palus region of Mars. The western part is dominated by lava flows of the Tharsis region. The central part includes ridged terrain of Lunae Planum. The west and north borders of Lunae Planum are dissected by the large, relatively young outflow channel, Kasei Vallis, which terminates in Chryse Planitia. Latitude range 0 to 30 degrees, longitude range 45 to 90 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03284-04high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03284-04high.jpg.html
Mars digital-image mosaic merged with color of the MC-9 quadrangle, Tharsis region of Mars. Three of the four largest shield volcanoes on Mars--Olympus, Ascraeus, and Pavonis Montes--lie within the Tharsis quadrangle, together with several smaller shields. The north-central part is marked by highly faulted terrain of Ceraunius Fossae. Latitude range 0 to 30 degrees, longitude range 90 to 135 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03284-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-03284-03high.jpg.html
Mars digital-image mosaic merged with color of the MC-8 quadrangle, Amazonis region of Mars. The central part, which is dominated by light-colored, relatively smooth to hummocky plains of Amazonis Planitia, is partly bounded to the east by the western flank of the largest known volcano in the solar system, Olympus Mons, and its associated aureole deposits. Moderately cratered knobby terrain is west of the plains of Amazonis Planitia. Latitude range 0 to 30 degrees, longitude range 135 to 180 degrees.
Dans l'album Surface de Mars depuis l'espace]]> photo Tue, 07 Sep 2010 14:21:02 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-04high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-04high.jpg.html
Center of the orthographic projection is at latitude 30 degrees S., longitude 330 degrees. Heavily cratered highlands dominate this view. Toward the lower right, a conspicuous light-colored circular depression marks the ancient large Hellas impact basin. Directly northeast of Hellas, several large ancient impacts dot the landscape, including Cassini, Schiaparelli, and Huygens. Several large outflow channels are located in the upper left-hand corner. The permanent, residual south polar ice cap is located near the bottom.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-03high.jpg.html
Center of the orthographic projection is at latitude 30 degrees S., longitude 210 degrees. Toward the top, the lowland plains of Elysium and Utopia Planitiae are separated from the darker heavily cratered highlands by a broad escarpment. The far bottom left is marked by the large light-colored ancient Hellas impact basin. The permanent south polar residual ice cap is located near the bottom.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-02High.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-02High.jpg.html
Center of the orthographic projection is at latitude 30 degrees S., longitude 90 degrees. The top half is dominated by the Tharsis Montes volcanoes, the large Alba Patera shield volcano, the dark Chryse basin, and a vast canyon system, Valles Marineris. In the central part, a prominent physiographic feature, Thaumasia plateau, includes a complex array of small- and large-scale faults and ridges and ancient volcanoes. The large conspicuous Argyre basin, southeast of the Thaumasia plateau, contains a broad expanse of light-colored plains 800 km across. The permanent south polar ice cap is located near the bottom.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03280-01high.jpg.html
Mars digital-image mosaic merged with color of the MC-30 quadrangle, Mare Australe region of Mars. The central part is dominated by a permanent residual ice cap that is enclosed by layered and troughed terrain. This cap is much smaller than the northern ice cap due to differing amounts of solar heating. The layered and troughed terrain is encircled by heavily and moderately cratered terrains that include unique depositional and erosional landforms, including large pits, troughs, and complex ridge systems. Latitude range -90 to -60 degrees, longitude range -180 to 180 degrees.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03270-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03270-02high.jpg.html
Mars digital-image mosaic merged with color of the MC-1 quadrangle, Mare Boreum region of Mars. The central part is covered by a residual ice cap that is cut by spiral-patterned troughs exposing layered terrain. The cap is surrounded by broad flat plains and large dune fields. Latitude range 65 to 90, longitude range -180 to 180.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03270-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03270-01high.jpg.html
Center of the orthographic projection is at latitude 30 degrees N., longitude 150 degrees. The north polar residual ice cap, which is cut by spiral-patterned troughs and surrounded by the dark lowland plains of Vastitas Borealis, is located at the top. The right-central part is dominated by the Tharsis Montes volcanoes. The most prominent of the Tharsis Montes volcanoes is the largest known volcano in the solar system, Olympus Mons. The light-colored lowland plains of Amazonis, Elysium, and Arcadia Planitiae lies north and west of Olympus Mons. The heavily cratered highlands dominate the lower one-third.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-05high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-05high.jpg.html
About 1000 Viking Orbiter red- and violet-filter images have been processed to provide global color coverage of Mars at a scale of 1 km/pixel. Individual image frames acquired during a single spacecraft revolution were first processed through radiometric calibration, cosmetic cleanup, geometric control, reprojection, and mosaicing. We have produced a total of 57 "single-rev" mosaics. All of the mosaics are geometrically tied to the Mars Digital Image Mosaic, a black-and-white base map with a scale of 231 m/pixel. We selected a subset of single-rev mosaics that provide the best global coverage (least atmospheric obscuration and seasonal frost); photometric normalization was applied to remove atmospheric effects and normalize the variations in illumination and viewing angles. Finally, these normalized mosaics were combined into global mosaics. Global coverage is about 98% complete in the red-filter mosaic and 95% complete in the violet-filter mosaic. Gaps were filled by interpolation. A green-filter image was synthesized from an average of the red and violet filter data to complete a 3-color set. The Viking Orbiters acquired actual green-filter images for only about half of the Martian surface. The final mosaic has been reprojected into several map projections. The orthographic view shown here is centered at 20 degrees latitude and 60 degrees longitude. The orthographic view is most like the view seen by a distant observer looking through a telescope. The color balance selected for these images was designed to be close to natural color for the bright reddish regions such as Tharsis and Arabia, but the data have been "stretched" such that the relatively dark regions appear darker and less reddish that their natural appearance. This stretching allows us to better see the color and brightness variations on Mars, which are related to the composition or physical structure of the surface materials, which include volcanic lava flows, wind- and water-deposited sedimentary rocks, and (at the poles) ice caps. The north polar cap is visible in this projection at the top of the image, the great equatorial canyon system (Valles Marineris) below center, and four huge Tharsis volcanoes (and several smaller ones) at left. Also note heavy impact cratering of the highlands (bottom and right portions of this mosaic) and the younger, less heavily cratered terrains elsewhere.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-04high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-04high.jpg.html
Center of the orthographic projection is at latitude 30 degrees N., longitude 30 degrees. The north polar residual ice cap, which is cut by spiral-patterned troughs, is located at the top. The central part is characterized by a dark depression, Chryse basin, where several large outflow channels terminate. The lower-left corner is marked by a vast system of canyons, Valles Marineris, which extends eastward for several thousand kilometers.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-03high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-03high.jpg.html
The coordinates of the Lambert azimuthal equal area projection are latitude 90 degrees N. to 90 degrees S. and longitude 0 degree to 180 degrees. Both polar residual ice caps are seen at top and bottom. The central part is dominated by the four largest and youngest volcanoes on Mars--Olympus, Arsia, Pavonis, and Ascraeus Montes--and by a vast system of canyons several thousand kilometers long--Valles Marineris. Directly to the northeast of Valles Marineris, several large outflow channels terminate at a dark depression, Chryse basin. The lower-right corner is marked by the large Argyre basin, defined by an expanse of light-colored plains 800 km across.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-02high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-02high.jpg.html
Center of the orthographic projection is at latitude 30 degrees N., longitude 270 degrees. The north polar residual ice cap of the Planum Boreum region, which is cut by spiral-patterned troughs, is located at top. The upper part is marked by a large depression, Isidis basin, which contains light-colored plains. The upper part also includes the light-colored smooth plains of Elysium Planitia and dark plains of Vastitas Borealis. Together, these form a vast expanse of contiguous plains. Toward the bottom, on the other hand, the southern hemisphere is almost entirely made up of heavily cratered highlands. At bottom left, a conspicuous, relatively bright circular depression marks the ancient large Hellas impact basin.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-01high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/VueGlo/003-03260-01high.jpg.html
The coordinates of the Lambert azimuthal equal area projection are latitude 90 degrees N. to 90 degrees S. and longitude -180 degrees to 0 degrees. The north polar residual ice cap of the Planum Boreum region, which is cut by spiral-patterned troughs, is located at top. The upper part is marked by large depression, Isidis basin, which contains light-colored plains. The upper part also includes the light-colored smooth plains of Elysium Planitia and dark plains of Vastitas Borealis. Together, these form a vast expanse of contiguous plains. Toward the bottom, on the other hand, the southern hemisphere is almost entirely made up of heavily cratered highlands. Toward the bottom, a conspicuous, relatively bright circular depression marks the ancient large Hellas impact basin.
Dans l'album Vues Globales de Mars]]> photo Tue, 07 Sep 2010 14:20:22 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/003-08129-28high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/003-08129-28high.jpg.html
Olympus Mons is the largest volcano in the Solar System and is thought to be quite young (compared to other features on Mars). So, what happens to all those lava flows running off of Olympus Mons? This observation shows that they are buried by yet younger "flood" lavas that lap up against the side of Olympus Mons. In this image we see two very different types of Olympus Mons lava flows. On the West, there is a thick flow with a rough surface texture. This is almost assuredly similar to lava flows in Hawaii that are called "aa." The lava is quite sticky as it flows and thus is ripped into chunks when it tries to move. Next to the aa flow is a long trough or channel. If you look closely, you can see tongues of lava flowing to either side of the channel. This looks like the product of a long eruption with lots of pulses. The channel eventually disappears and an irregular set of pits is visible at its extension. This is probably because the channel had developed a solid roof (becoming a lava tube) and then lava burst out of the tube. This kind of complex evolution of a lava flow can be seen on Kilauea Volcano, in Hawaii, today. But, happily, it is happening at a much smaller scale than these ancient lava flows on Mars.
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Mon, 06 Sep 2010 11:18:20 +0200 http://www.cieletespacephotos.fr/main.php/v/Actus/003-08129-27high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Actus/003-08129-27high.jpg.html
These cones are similar in size and shape to cones found in Iceland where hot lava has run over wet ground. The heat from the lava boils the water which bursts through the lava flow. These steam-driven exploding bubbles of lava throw chunks of molten and solid lava into the air. A long series of such explosions is needed to build up one of the large cones. The cones appear in chains because the surface of the lava flow was moving while the series of explosions were taking place. This is sort of like a miniature version of how the Hawaiian Island chain forms. The hot spot under Hawaii is fixed but the Earth's crust slides past it.
Dans l'album L'ACTUALITE EN IMAGES : Les toutes dernières images des observatoires et des astrophotographes...]]> photo Mon, 06 Sep 2010 11:18:20 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-29high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-29high.jpg.html
This image shows portions of an alluvial fan complex in Harris Crater, an approximately 83-kilometer diameter crater located on the Northern rim of the Hellas Basin. An alluvial fan is a fan-shaped accumulation of loose, water-transported material deposited where an upland drainage emerges into a low-relief basin. In this case, two source regions on the Northern crater rim fed discrete lobe deposits that make up the alluvial fan complex. These lobes have different surface textures that enable researchers to map out the different components of the fan and investigate the sequence of fan-building processes that operated in the past. The fan surfaces have experienced erosional degradation, presumably the result of wind. One interesting result of this is the formation of "inverted channels," where the former channel floors are now preserved as ridges. Tributary channels on the alluvial fan were armored by coarse gravels or chemically cemented, making the channel bottoms resistant to erosion. Over time, natural erosion from wind and other processes left the inverted channels elevated above the surrounding terrain. The inverted channels record the former flow direction. Differences in channel orientation point to different source regions. The HiRISE image shows that this material is boulder-rich, which suggests the material was transported in a debris flow (a sediment-concentrated slurry of material). The preserved landforms record episodic fan formation (different portions of the fan were active at different times) resulting from different fluid flow processes. The transition from fluvial to late-stage debris flow(s) suggests a decline in available water and/or change in sediment supply. In-depth geologic investigations, such as this one, help refine our understanding of the relative timing and necessary climatic conditions required at the time this alluvial fan formed.
Dans l'album Surface de Mars depuis l'espace]]> photo Mon, 06 Sep 2010 11:18:03 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-28high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-28high.jpg.html
Olympus Mons is the largest volcano in the Solar System and is thought to be quite young (compared to other features on Mars). So, what happens to all those lava flows running off of Olympus Mons? This observation shows that they are buried by yet younger "flood" lavas that lap up against the side of Olympus Mons. In this image we see two very different types of Olympus Mons lava flows. On the West, there is a thick flow with a rough surface texture. This is almost assuredly similar to lava flows in Hawaii that are called "aa." The lava is quite sticky as it flows and thus is ripped into chunks when it tries to move. Next to the aa flow is a long trough or channel. If you look closely, you can see tongues of lava flowing to either side of the channel. This looks like the product of a long eruption with lots of pulses. The channel eventually disappears and an irregular set of pits is visible at its extension. This is probably because the channel had developed a solid roof (becoming a lava tube) and then lava burst out of the tube. This kind of complex evolution of a lava flow can be seen on Kilauea Volcano, in Hawaii, today. But, happily, it is happening at a much smaller scale than these ancient lava flows on Mars.
Dans l'album Surface de Mars depuis l'espace]]> photo Mon, 06 Sep 2010 11:18:03 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-27high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-27high.jpg.html
These cones are similar in size and shape to cones found in Iceland where hot lava has run over wet ground. The heat from the lava boils the water which bursts through the lava flow. These steam-driven exploding bubbles of lava throw chunks of molten and solid lava into the air. A long series of such explosions is needed to build up one of the large cones. The cones appear in chains because the surface of the lava flow was moving while the series of explosions were taking place. This is sort of like a miniature version of how the Hawaiian Island chain forms. The hot spot under Hawaii is fixed but the Earth's crust slides past it.
Dans l'album Surface de Mars depuis l'espace]]> photo Mon, 06 Sep 2010 11:18:03 +0200 http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-26high.jpg.html http://www.cieletespacephotos.fr/main.php/v/SystemeSolaire/Mars/SurfaceMar/003-08129-26high.jpg.html
This scene shows the curving, Eastern interior walls of a 12 kilometer-diameter (approximately 7.4 mile-diameter) impact crater in the Southern mid-latitudes of Mars. The sun is off-scene to the Northwest (left in the map-projected images), causing the Northwestern wall to cast a shadow far into the deep crater interior. This shadowing effect also highlights the gullies incised into the Northern wall of the crater. Many ideas have been advanced as to how such gullies form - some appear to have involved flowing water, perhaps from melting ice, while others appear to be formed solely due to mass wasting of soil and rocks. In the enhanced-color strip down the middle of this image, the Northern wall displays some bluish-purplish coating, which is seasonal frost that remains deposited on such steep slopes facing away from the equator at this time of year, much like frost often accumulates first, or disappears last, from mountain slopes on Earth that face away from the equator (North-facing in the Northern Hemisphere, and South-facing in the Southern Hemisphere).
Dans l'album Surface de Mars depuis l'espace]]> photo Mon, 06 Sep 2010 11:18:03 +0200 http://www.cieletespacephotos.fr/main.php/v/Univers/Supernova/023-00400-13high.jpg.html http://www.cieletespacephotos.fr/main.php/v/Univers/Supernova/023-00400-13high.jpg.html
An international team of astronomers using the Hubble Space Telescope reports a significant brightening of the emissions from Supernova 1987A. The results, which appear in this week's Science magazine, are consistent with theoretical predictions about how supernovae interact with their immediate galactic environment. The team observed the supernova remnant in optical, ultraviolet, and near-infrared light. They studied the interaction between the ejecta from the stellar explosion and a glowing 6-trillion-mile-diameter ring of gas encircling the supernova remnant. The gas ring was probably shed some 20,000 years before the supernova exploded. Shock waves resulting from the impact of the ejecta onto the ring have brightened 30 to 40 pearl-like "hot spots" in the ring. These blobs likely will grow and merge together in the coming years to form a continuous, glowing circle. Discovered in 1987, Supernova 1987A is the closest exploding star to Earth to be detected since 1604 and it resides in the nearby Large Magellanic Cloud, a dwarf galaxy adjacent to our own Milky Way Galaxy.
Dans l'album Les supernovas]]> photo Mon, 06 Sep 2010 11:17:31 +0200