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Zusammenstellung ausgewählter Bilder zu den Asteroiden, die um weiterführenden Links mit der Möglichkeit des Downloads ergänzt wurden.

  • Eros, Mosaik der nördlichen Hemisphäre

    Eros, Mosaik der nördlichen Hemisphäre

    While NEAR Shoemaker orbits Eros, the asteroid appears too large for the camera's field of view. In order to get a complete view of the surface from a particular vantage point, several images are mosaiced. To do this, the digital images returned by the spacecraft are draped over a computer model of the asteroid's shape.

    This spectacular view -- looking down on the north polar region -- was constructed from six images taken February 29, 2000, from an orbital altitude of about 200 kilometers (124 miles). This vantage point highlights the major physiographic features of the northern hemisphere: the saddle seen at the bottom; the 5.3-kilometer (3.3-mile) diameter crater at the top; and a major ridge system running between the two features that spans at least one-third of the asteroid's circumference.

    Bild: NASA/JPL/JHUAPL

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  • Eros, Mosaik aus vier Aufnahmen

    Eros, Mosaik aus vier Aufnahmen

    This picture of Eros, the first of an asteroid taken from an orbiting spacecraft, is a mosaic of four images obtained by NEAR on February 14, 2000, immediately after the spacecraft's insertion into orbit. We are looking down over the north pole of Eros at one of the largest craters on the surface, which measures 4 miles (6 kilometers) across. Inside the crater walls are subtle variations in brightness that hint at some layering of the rock in which the crater formed. Narrow grooves that run parallel to the long axis of Eros cut through the southeastern part of the crater rim. A house-sized boulder is present near the floor of the crater; it appears to have rolled down the bowl-shaped crater wall. A large number of boulders is also present on other parts of the asteroid's surface. The surface of the asteroid is heavily cratered, indicating that Eros is relatively old.

    Bild: NASA/JPL/JHUAPL

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  • Asteroid Steins, aufgenommen von Rosetta

    Asteroid Steins, aufgenommen von Rosetta

    Asteroid Steins seen from a distance of 800 km, taken by the OSIRIS imaging system from two different perspectives. The effective diameter of the asteroid is 5 km, approximately as predicted. At the top of the asteroid (as shown in this image), a large crater, approximately 1.5-km in size, can be seen. Scientists were amazed that the asteroid survived the impact that was responsible for the crater.

    Bild: ESA ©2008 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA

  • Lutetia, Detail der Oberfläche mit einem Erdrutsch

    Lutetia, Detail der Oberfläche mit einem Erdrutsch

    Landslides on Lutetia are thought to have been caused by the vibrations created by impacts elsewhere on the asteroid dislodging pulverised rocks.

    Bild: ESA 2011 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA

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  • Lutetia, globale Ansicht mit Kennzeichnung der großen Krater und der durch sie verursachten Gräben

    Lutetia, globale Ansicht mit Kennzeichnung der großen Krater und der durch sie verursachten Gräben

    Looking face on at the North Pole Crater Cluster (purple outline) on asteroid Lutetia, with Massilia to the lower left (red outline). Marked on the image are the concentric grooves or ‘lineaments’ associated with the large craters. The lineaments coloured blue infer the presence of a large crater – nicknamed Suspicio – on the unseen portion of Lutetia. Yellow denotes lineaments not associated with any of the craters discussed in this study.

    Lutetia was imaged in July 2010 by ESA’s Rosetta spacecraft, while en route to Comet 67P/Churyumov-Gerasimenko. Rosetta took images of the 100 km-wide asteroid for about two hours during the flyby. At its closest approach, Rosetta was 3162 km from Lutetia. In the image shown here, north is towards the observer.

    Bild: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

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  • Gaspra, hochauflösendes Mosaik aus zwei Einzelbildern

    Gaspra, hochauflösendes Mosaik aus zwei Einzelbildern

    This picture of asteroid 951 Gaspra is a mosaic of two images taken by the Galileo spacecraft from a range of 5,300 kilometers (3,300 miles), some 10 minutes before closest approach on October 29, 1991. The Sun is shining from the right; phase angle is 50 degrees. The resolution, about 54 meters/pixel, is the highest for the Gaspra encounter and is about three times better than that in the view released in November 1991. Additional images of Gaspra remain stored on Galileo's tape recorder, awaiting playback in November. Gaspra is an irregular body with dimensions about 19 x 12 x 11 kilometers (12 x 7.5 x 7 miles). The portion illuminated in this view is about 18 kilometers (11 miles) from lower left to upper right. The north pole is located at upper left; Gaspra rotates counterclockwise every 7 hours. The large concavity on the lower right limb is about 6 kilometers (3.7 miles) across, the prominent crater on the terminator, center left, about 1.5 kilometers (1 mile). A striking feature of Gaspra's surface is the abundance of small craters. More than 600 craters, 100-500 meters (330-1650 feet) in diameter are visible here. The number of such small craters compared to larger ones is much greater for Gaspra than for previously studied bodies of comparable size such as the satellites of Mars. Gaspra's very irregular shape suggests that the asteroid was derived from a larger body by nearly catastrophic collisions. Consistent with such a history is the prominence of groove-like linear features, believed to be related to fractures. These linear depressions, 100-300 meters wide and tens of meters deep, are in two crossing groups with slightly different morphology, one group wider and more pitted than the other. Grooves had previously been seen only on Mars's moon Phobos, but were predicted for asteroids as well. Gaspra also shows a variety of enigmatic curved depressions and ridges in the terminator region at left.

    Bild: NASA/JPL

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  • Gaspra im Vergeich mit den beiden Marsmonden Deimos und Phobos

    Gaspra im Vergeich mit den beiden Marsmonden Deimos und Phobos

    This montage shows asteroid 951 Gaspra (top) compared with Deimos (lower left) and Phobos (lower right), the moons of Mars. The three bodies are shown at the same scale and nearly the same lighting conditions. Gaspra is about 17 kilometers (10 miles) long. All three bodies have irregular shapes, due to past catastrophic conditions. However their surfaces appear remarkably different, possibly because of differences in composition but most likely because of very different impact histories. The Phobos and Deimos images were obtained by the Viking Orbiter spacecraft in 1977; the Gaspra image is the best of a series obtained by the Galileo spacecraft on October 29, 1991. Galileo is scheduled to add the detailed view of another asteroid when it flies by Ida in August 1993. The Galileo project, whose primary mission is the exploration of the Jupiter system in 1995-97, is managed for NASA's Office of Space Science and Applications by the Jet Propulsion Laboratory.

    Bild: NASA/JPL

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  • Farbansicht des Asteroiden 243 Ida und mit seinem Mond Dactyl

    Farbansicht des Asteroiden 243 Ida und mit seinem Mond Dactyl

    This color picture is made from images taken by the imaging system on the Galileo spacecraft about 14 minutes before its closest approach to asteroid 243 Ida on August 28, 1993. The range from the spacecraft was about 10,500 kilometers (6,500 miles). The images used are from the sequence in which Ida's moon was originally discovered; the moon is visible to the right of the asteroid. This picture is made from images through the 4100-angstrom (violet), 7560 A (infrared) and 9680 A (infrared) filters. The color is 'enhanced' in the sense that the CCD camera is sensitive to near infrared wavelengths of light beyond human vision; a 'natural' color picture of this asteroid would appear mostly gray. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body as well as subtle color variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the center of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near infrared light, suggesting a difference in the abundance or composition of iron-bearing minerals in these areas. Ida's moon also has a deeper near-infrared absorption and a different color in the violet than any area on this side of Ida. The moon is not identical in spectral properties to any area of Ida in view here, though its overall similarity in reflectance and general spectral type suggests that it is made of the same rock types basically. These data, combined with study of further imaging data and more detailed spectra from the Near Infrared Mapping Spectrometer, may allow scientists to determine whether the larger parent body of which Ida, its moon, and some other asteroids are fragments was a heated, differentiated object or made of relatively unaltered primitive chondritic material.

    Bild: NASA/JPL

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  • Ida, neun verschiedene Ansichten in Echtfarbe

    Ida, neun verschiedene Ansichten in Echtfarbe

    This set of color images of asteroid 243 Ida was taken by the imaging system on the Galileo spacecraft as it approached and raced past the asteroid on August 28, 1993. These images were taken through the 4100-angstrom (violet), 7560-angstrom (infrared) and 9680- angstrom (infrared) filters and have been processed to show Ida as it would appear to the eye in approximately natural color. The stark shadows portray Ida's irregular shape, which changes its silhouetted outline when seen from different angles. More subtle shadings reveal surface topography (such as craters) and differences in the physical state and composition of the soil ("regolith"). Analysis of the images show that Ida is 58 kilometers long and 23 kilometers wide (36 x 14 miles). Ida is the first asteroid discovered to have a natural satellite, Dactyl (not shown here). Both Ida and Dactyl are heavily cratered by impacts with smaller asteroids and comets, including some of the same populations of small objects that bombard Earth. These data, combined with reflectance spectra from Galileo's near-infrared mapping spectrometer, may allow scientists to determine whether Ida is a relatively unaltered primitive object made of material condensed from the primordial Solar Nebula at the origin of the Solar System or whether it has been altered by strong heating--evidence interpreted so far suggests that Ida is a piece of a larger object that has been severely heated. Whereas heating and melting of large planets is well understood, the cause of heating of small asteroids is more enigmatic--it may have involved exotic processes that occurred only for a short time after the birth of the Sun and its planets.

    Bild: NASA/JPL

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  • Asteroid Annefrank, Komet Wild 2 und Komet Tempel 1

    Asteroid Annefrank, Komet Wild 2 und Komet Tempel 1

    This composite image shows the three small worlds NASA's Stardust spacecraft encountered during its 12 year mission. Stardust performed a flyby of asteroid Annefrank was visited on Nov. 2, 2002. Comet Wild 2 was visited by the spacecraft on Jan. 2, 2004. The comet Tempel 1 encounter occurred on Feb. 14, 2011.

    The flyby of asteroid Annefrank was used as a dress rehearsal of procedures the spacecraft would use for its upcoming encounter with its primary science target, comet Wild 2. Stardust passed within about 3,300 kilometers (2,050 miles) of the asteroid.

    During the comet Wild 2 encounter, Stardust flew within about 230 kilometers (143 miles) of the comet, catching samples of comet particles and scoring detailed pictures of Wild 2's pockmarked surface. The collected particles were stowed in a sample return capsule onboard Stardust. The samples were returned to Earth for in-depth analysis on January 15, 2006, when the spacecraft's sample return capsule made a soft landing at the U.S. Air Force Utah Test and Training Range.

    Stardust flew within 181 kilometers (112 miles) of comet Tempel 1 during the spacecraft's final close encounter. During the Tempel 1 flyby, the spacecraft took images of the comet's surface to observe what changes occurred since a NASA spacecraft last visited. (NASA's Deep Impact spacecraft executed an encounter with Tempel 1 in July 2005).

    Bild: NASA/JPL-Caltech/University of Maryland/Cornell

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  • Vesta, globales Mosaik

    Vesta, globales Mosaik

    As NASA's Dawn spacecraft takes off for its next destination, this mosaic synthesizes some of the best views the spacecraft had of the giant asteroid Vesta. Dawn studied Vesta from July 2011 to September 2012. The towering mountain at the south pole -- more than twice the height of Mount Everest -- is visible at the bottom of the image. The set of three craters known as the "snowman" can be seen at the top left.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vollständige Ansicht von Vesta

    Vollständige Ansicht von Vesta

    NASA's Dawn spacecraft obtained this image with its framing camera on July, 24 2011. This image was taken through the camera's clear filter. The image has a resolution of about 485 meters per pixel.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vesta, Abhang im Südpolgebiet

    Vesta, Abhang im Südpolgebiet

    NASA's Dawn spacecraft obtained this image with its framing camera on August 12, 2011. The image was taken through the framing camera's clear filter. The image has a resolution of about 260 meters per pixel.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vesta, topographische Bildkarte des Südpols mit farbkodierter Höhe

    Vesta, topographische Bildkarte des Südpols mit farbkodierter Höhe

    This false-color map of the giant asteroid Vesta was created from stereo images obtained by the framing camera aboard NASA's Dawn spacecraft. The image shows the elevation of surface structures with a horizontal resolution of about 750 meters per pixel.

    The terrain model of Vesta's southern hemisphere shows a big circular structure with a diameter of about 300 miles (500 kilometers), its rim rising above the interior of the structure for more than 9 miles (15 kilometers.) From low-resolution images of the Hubble Space Telescope it was known that a big depression existed at Vesta's south pole, suggestive of being a big impact basin. Scientists on the Dawn team are still investigating the processes that formed this structure.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vesta, Mosaik des Südpols

    Vesta, Mosaik des Südpols

    This image obtained by the framing camera on NASA's Dawn spacecraft shows the south pole of the giant asteroid Vesta.

    Scientists are discussing whether the circular structure that covers most of this image originated by a collision with another asteroid, or by internal processes early in the asteroid's history. Images in higher resolution from Dawn's lowered orbit might help answer that question.

    The image was recorded with the framing camera aboard NASA's Dawn spacecraft from a distance of about 1,700 miles (2,700 kilometers). The image resolution is about 260 meters per pixel.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vesta, perspektivische Ansicht der Gräben im System Divalia Fossa

    Vesta, perspektivische Ansicht der Gräben im System Divalia Fossa

    This image from NASA's Dawn mission shows huge grooves on the giant asteroid Vesta that were the result of mega impacts at the south pole. As Dawn sent the first close-up images of Vesta back to Earth in July 2011, scientists immediately noticed numerous grooves, as if created by a gigantic plow. This image shows two grooves in the Divalia Fossa system, running parallel to the lower edge of the image.

    The majority of these grooves extend along the equator, but a second group -- inclined with respect to the equator -- have been identified in the northern hemisphere. These parallel trenches are usually several hundred miles (kilometers) long, up to 9 miles (15 kilometers) wide and more than a half mile (1 kilometer) deep. They are the result of two large asteroid impacts far in the southern hemisphere, demonstrating that impact events that occurred hundreds of miles (kilometers) apart caused shocks throughout Vesta and altered its surface.

    The scene is an artificially generated oblique view of the grooves (or troughs) that run along Vesta's equator. The image was rendered from a global mosaic of Vesta processed from thousands of individual images obtained by the framing camera between January and April 2012. The altitude was approximately 130 miles (210 kilometers) above Vesta's surface. The image resolution is about 70 feet (20 meters) per pixel.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Vesta, die

    Vesta, die "Schneemann"-Krater Marcia, Calpurnia und Minucia

    Three impact craters of different sizes, arranged in the shape of a snowman, make up one of the most striking features on Vesta, as seen in this view from NASA's Dawn mission. In this view the three "snowballs" are upside down, so that the shadows make the features easily recognizable. North is to the lower right in the image, which has a resolution of 230 feet (70 meters) per pixel.

    The image is composed of many individual photographs taken between October and December 2011 by Dawn's framing camera. They were obtained during the high-altitude mapping orbit, at about 420 miles (680 kilometers) above Vesta's surface.

    The largest of the three craters, Marcia, has a diameter of about 40 miles (60 kilometers). The central crater, which is about 30 miles (50 kilometers) in diameter, is named Calpurnia, and the lower crater, named Minucia, has a diameter of about 14 miles (22 kilometers). Marcia and Calpurnia are possibly the result of an impact by doublet asteroids, whereas Minucia was formed by a later impact.

    Bild: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

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  • Bennu, 3D-Modell mit Albedokarte und globalem Bildmosaik

    Bennu, 3D-Modell mit Albedokarte und globalem Bildmosaik

    3d model of asteroid Bennu with albedo map and global image mosaic.

    Bild: NASA's Scientific Visualization Studio
    Data provided by NASA/University of Arizona/CSA/York University/Open University/MDA.

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  • Asteroid Ruygu, komplette Ansicht

    Asteroid Ruygu, komplette Ansicht

    Asteroid Ryugu photographed with the ONC-T from a distance of about 20 km. The image was taken at around 23:13 JST on June 30, 2018.

    Bild: JAXA, University of Tokyo, Kochi University, Rikkyo University, Nagoya University, Chiba Institute of Technology, Meiji University, University of Aizu and AIST

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  • Asteroid Ryugu, Detail der Oberfläche aus 64 m Entfernung

    Asteroid Ryugu, Detail der Oberfläche aus 64 m Entfernung

    When Hayabusa2 descended towards Ryugu for the MINERVA-II1 deployment operation, the ONC-T (Optical Navigation Camera - Telescopic) captured images at the highest resolution to date.

    Image of Ryugu captured by the ONC-T at an altitude of about 64m. Image was taken on September 21, 2018 at around 13:04 JST.This is the highest resolution photograph obtained of the surface of Ryugu. Bottom left is a large boulder.

    Bild:JAXA, University of Tokyo, Kochi University, Rikkyo University, Nagoya University, Chiba Institute of Technology, Meiji University, Aizu University, AIST

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  • Asteroid Ryugu, Teleaufnahme der ONC

    Asteroid Ryugu, Teleaufnahme der ONC

    Asteroid Ryugu from an altitude of 6km. Image was captured with the Optical Navigation Camera - Telescopic (ONC-T) on July 20, 2018 at around 7:12 UTC.

    Bild: JAXA, University of Tokyo, Kochi University, Rikkyo University, Nagoya University, Chiba Institute of Technology, Meiji University. University of Aizu, AIST

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