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In a first, ESA's Mars Express orbiter imaged the martian moons Phobos and Deimos together on 5 November 2009. Apart from their 'wow' factor, these unique images will help the HRSC team validate and refine existing orbit models of the two moons. The images were acquired with the Super Resolution Channel (SRC) of the High Resolution Stereo Camera (HRSC). The camera took 130 images of the moons on 5 November at 9:14 CET in a span of 1.5 minutes at intervals of 1s, speeding up to 0.5-s intervals toward the end. The image resolution is 110 m/pixel for Phobos and 240 m/pixel for Deimos -- Deimos was more than twice as far from the camera. The Super Resolution Channel of the HRSC uses an additional lens, which has a very narrow field of view of just 0.5°, providing four times the magnification than otherwise providing four times the resolution of the HRSC colour stereo channel. Phobos, the larger of the two moons, orbits closer to the Red Planet, circling it every 7 hours and 39 minutes. It travels faster relative to Mars than the Moon relative to Earth. It was 11800 km from Mars Express when the images were taken. Deimos was 26200 kilometres away. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Pioneering images of both martian moons
This simulated voyage over the surface of Neptune's large moon Triton was produced using topographic maps derived from images acquired by NASA's Voyager spacecraft during its August 1989 flyby, 20 years ago this week. Triton was the last solid object visited by the Voyager 2 spacecraft on its epic 10-year tour of the outer solar system. Voyager mapped only the hemisphere that faces Neptune, but revealed a very young surface scarred by rising blobs of ice (diapirs), faults, and volcanic pits and lava flows composed of water and other ices. The video begins near the western edge of this hemisphere with an approach over cantaloupe terrain and two large smooth walled plains. The video tracks due east for roughly 1500 kilometers over a large province of volcanic pits, calderas and smooth plains. As can be seen in this video, Triton is locally very rugged (with pits and mounds that are typically a few hundred meters [several hundred feet] high), but has no large mountains or deep basins and regional relief is low. The lack of large topographic features is a consequence of Triton's high internal heat and the low strength of most ices. The video was produced by using a new topographic map of Triton, combined with a 1.65-kilometer resolution image mosaic. Topographic mapping was based on shape-from-shading analysis of the original Voyager images. Vertical relief has been exaggerated by a factor of 25 to aid interpretation. Credit: NASA/JPL/Universities Space Research Association/Lunar & Planetary Institute
 
 
Flight Over Triton
This movie shows one cycle of pulsed gamma rays from the Vela pulsar as constructed from photons detected by Fermi's Large Area Telescope. The movie includes data from August 4 to Sept. 15, 2008. The bluer color in the latter part of the pulse indicates the presence of gamma rays with energies exceeding a billion electron volts. For comparison, visible light has energies between two and three electron volts. Credit: NASA/DOE/Fermi LAT Collaboration
 
 
Vela Pulsar in Gamma Rays
Conceptual animation and data visualization showing how the two simultaneous sets of images from the STEREO-A and STEREO-B spacecraft are used to determine the three-dimensional shape of a coronal mass ejection. Credit: Walt Feimer, NASA
 
 
Anatomy of a Coronal Mass Ejection
Did Mars once have an environment capable of supporting life? NASA's next rover will further unravel that mystery. Credit: NASA/JPL/Caltech
 
 
Mars Science Laboratory Overview
This animation demonstrates how the rover will enter, descend and land on the surface of Mars. Credit: NASA/JPL/Caltech
 
 
Mars Science Laboratory Mission Animation
Credit: Cornell University
 
 
Stardust-NExT Flyby of Comet Tempel 1 on February 14, 2011
This all-sky movie shows Fermi LAT counts of gamma rays with energies greater than 300 million electron volts from August 4 to October 30, 2008. Brighter colors indicate brighter gamma-ray sources. The circles show the northern (left) and southern galactic sky. Their edges lie along the plane of our galaxy, the Milky Way. Credit: NASA/DOE/Fermi LAT Collaboration
 
 
Fermi All-sky Movie Shows Flaring, Fading Blazars
The STEREO spacecraft are entering the L4 and L5 Lagrangian point regions. L4 and L5 are where the combined gravity of the sun and Earth balance the forces from the object's orbital motion. Scientists believe these places may hold small asteroids which could be leftovers from the formation of the solar system. STEREO will be imaging these regions in an attempt to detect these asteroids. Credit: NASA
 
 
L4 and L5 Points in the STEREO Orbit
This artist's animation illustrates how the dust cover on NASA's Kepler telescope will be ejected. Engineers will send a command up to the space telescope to pass an electrical current through a
 
 
Taking the Lid Off Kepler
Glowing like a neon lasso, Saturn’s aurora is seen spinning above Saturn’s north pole over the course of most of a Saturn day in this movie made from multiple images taken by the ultraviolet imaging spectrograph on NASA’s Cassini spacecraft. Credit: NASA/JPL/University of Colorado/Central Arizona College
 
 
Ultraviolet Aurora Movie
Cassini's radar mapper has obtained stereo views of close to 2 percent of Titan's surface during 19 flybys over the last five years. The process of making topographic maps from images is just getting started, but the results already reveal some of the diversity of Titan's geologic features. Credit: NASA/JPL/USGS
 
 
Hotei
Cassini's radar mapper has obtained stereo views of close to 2 percent of Titan's surface during 19 flybys over the last five years. The process of making topographic maps from images is just getting started, but the results already reveal some of the diversity of Titan's geologic features. Credit: NASA/JPL/USGS
 
 
Ganesa Macula
Comparisons with computer simulations suggest that the observations of a remote galaxy which presents very peculiar motions, as revealed by Hubble and ESO's Very Large Telescope, can be explained by the collision of two spiral galaxies. The simulations shows how the two galaxies merge to produce a galaxy looking similar to what the NASA/ESA Hubble Space Telescope observed, and with internal motions similar to what the FLAMES/GIRAFFE spectrograph revealed. Credit: ESO/J. Barnes/Peirani et al.
 
 
Galaxies in collision
The GOCE (Gravity Field and steady-state Ocean Circulation Explorer) mission is dedicated to measuring the Earth's gravity field and modelling the geoid with unprecedented accuracy and spatial resolution. Since the satellite has to be completely stable to ensure the acquisition of true gravity readings, the spacecraft has no mechanical moving parts. In order to receive the optimum gravity signal GOCE will fly in a particularly low orbit of just 250 km above the surface of the Earth. The slim, octagonal, spacecraft is about 5 m in length and 1 m across – configured to keep aerodynamic drag and torque to an absolute minimum. Credits: ESA - AOES Medialab 2009
 
 
GOCE: Revealing an intimate portrait of Earth
This animation shows a computer simulation of the planet HD 80606b from an observer located at a point in space lying between the Earth and the HD 80606 system. The animation starts 2.2 days before the moment of close approach and ends 8.9 days later. The blue areas are reflected starlight (the blue color arises mainly from absorption by sodium and potassium in the planetary atmosphere). Red regions are areas of the planet that are glowing with their own intrinsic heat. The point of closest approach -- and maximum heating -- occurs about 4.5 seconds into the animation. As the planet whips around the star, we see the evolving thermal storm patterns across its unilluminated side. The planet's transit behind its star (as would be seen from Earth four seconds into the animation) is not shown in this simulation. These theoretical models allow astronomers to better understand weather patterns on distant planets. While direct telescopic observations of the atmospheres of such worlds may be many decades away, such simulations give us a clue to what we may see when it becomes possible. Credit: NASA/JPL-Caltech/UCSC
 
 
Tour of Planet with Extreme Temperature Swings
This visualization shows a fly-through of Cas A based on the 3-D representation constructed from Chandra and Spitzer data. It begins with an artists rendition of the neutron star previously detected by Chandra. Next, new features unseen in traditional 2-D data sets are visible, including details of how the parent star exploded. The green region is mostly iron observed in X-rays; the yellow region is mostly argon and silicon seen in X-rays, optical and infared; the red region is cooler debris seen in the infared and the blue region is the outer blast wave, most prominent in X-rays. Credit: NASA/CXC/D.Berry
 
 
3-D Fly-Through of Cassiopeia A
This brief movie of X-ray data from Chandra of Cas A was made by combining observations taken in January 2000, February 2002, February 2004, and December 2007. In these images, the lowest-energy X-rays Chandra detects are shown in red, intermediate energies in green, and the highest energies in blue. Scientists have used the movie to measure the expansion velocity of the leading edge of the explosion's outer blast wave (shown in blue). The researchers find that the velocity is 11 million miles per hour, which is significantly slower than expected for an explosion with the energy estimated to have been released in Cas A. Credit: NASA/CXC/SAO/D.Patnaude et al.
 
 
Brief Time-lapse Movie of Cassiopeia A
Interaction between Venus and the solar wind. Credit: ESA (Animation by C. Carreau)
 
 
Interaction between Venus and the solar wind
Change is detected on Saturn's moon Titan, in these three composite images from data taken during flybys in October 2005, January 2006 and March 2006. The change observed between flybys may be evidence of cryovolcanic activity—ice volcanoes—according to some Cassini scientists. Credit: NASA/JPL/University of Arizona
 
 
Titan's Chilly Volcanoes?
This simulated flyover shows rhythmic layers of sedimentary rock inside Becquerel crater on Mars. The animation uses three-dimensional modeling based on a stereo pair of images from the High Resolution Imaging Science Experiment (HiRISE) on NASA's Mars Reconnaissance Orbiter. Credit: NASA/JPL-Caltech/University of Arizona.
 
 
Flyover Animation of Becquerel Crater on Mars
This movie combines Swift UVOT observations of Comet 73P/Schwassmann-Wachmann 3's fragment C from May 1 to May 11, 2006. Look for blobs of dust moving down the comet's inner tail (orange and yellow). Credit: NASA/Swift/Stefan Immler and Dennis Bodewits.
 
 
Comet 73P
The movie begins with a view of how the surface looks today. A blue line is drawn on the image and an artist's concept then reveals what the ice may look like underneath. The movie was created using image data from the Context Camera on the Mars Reconnaissance Orbiter (MRO) spacecraft combined with results from the SHARAD radar sounder on MRO and HRSC digital elevation map from the Mars Express spacecraft. The color of the Martian surface and ice was estimated from MRO HiRISE color images of other Martian craters and the polar ice caps. The buried ice in these craters as measured by SHARAD is about 250 meter thick on the upper crater and about 300 and 450 meters on the middle and lower levels respectively. Each image is 20 km (12.8 mi.) across and extends to 50 km (32 mi) in the distance. Credit: NASA/JPL-Caltech/UTA/UA/MSSS/ESA/DLR/JPL Solar System Visualization Project
 
 
Mars Reconnaissance Orbiter Detects Buried Glaciers
This animation shows the 3D (shape) model of Mars' moon Phobos, built thanks to the data collected by Mars Express' High Resolution Stereo Camera (53 images obtained by the Super Resolution Channel, or SRC) and NASA's Viking (16 images). The model is dressed with a mosaic of the same images. The SRC coverage is about 70% of the moon's surface. The mean resolution is 12 m/pixel. Credits: ESA/DLR (K.Willner)/FU Berlin (G. Neukum)
 
 
Phobos 3D Model
There are certain spots in deep craters at the moon's poles where the sun may not have hit for billions of years. These areas, called Permanently Shadowed Regions, may be able to trap water molecules as ice. This video shows how even as the sun hits from different angles, some parts never receive light. Credit: NASA/JPL.
 
 
Lunar Landscape
In 1998 NASA's Lunar Prospector mission used the presence of hydrogen as a sign of potential ice deposits. As you can see in this video, Prospector data showed significantly more hydrogen at the south pole of the moon. LRO will build on this data and narrow down the regions that may contain water ice deposits. Credit: NASA's Goddard Space Flight Center's Scientific Visualization Studio.
 
 
Lunar Surface with Hydrogen Data
Animation of Hinode solar observations from Aug. 23, 2007. Credit: JAXA/NASA/NAOJ/STFC/ESA.
 
 
Hinode Solar Observations
Credit: NASA/Goddard Space Flight Center Conceptual Image Lab.
 
 
Solar Cycle
Artist's Concept of MAVEN, set to launch in 2013. Credit: NASA.
 
 
MAVEN
This animation shows how astronomers think GRB 080319B erupted. A narrow, ultrafast jet first punches through the star and is followed by a wider, less energetic jet. Credit: NASA/Swift/Cruz deWilde.
 
 
Gamma-ray burst
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