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        {
            "id": 5319,
            "url": "https://svs.gsfc.nasa.gov/5319/",
            "result_type": "Visualization",
            "release_date": "2024-06-24T16:20:00-04:00",
            "title": "Moon Essentials: Turntable",
            "description": "A model of the Moon displayed as a looping 360-degree turntable animation. || moon.0001_print.jpg (1024x576) [71.5 KB] || moon.0001_searchweb.png (320x180) [36.0 KB] || moon.0001_thm.png (80x40) [3.4 KB] || moon_turntable_1080p30.mp4 (1920x1080) [39.9 MB] || moon_turntable_720p30.mp4 (1280x720) [19.2 MB] || moon_turntable_360p30.mp4 (640x360) [5.0 MB] || tiff [128.0 KB] || exr [128.0 KB] || moon_turntable_2160p30.mp4 (3840x2160) [137.0 MB] || ",
            "hits": 241
        },
        {
            "id": 31194,
            "url": "https://svs.gsfc.nasa.gov/31194/",
            "result_type": "Hyperwall Visual",
            "release_date": "2022-10-04T00:00:00-04:00",
            "title": "DART: Double Asteroid Redirection Test",
            "description": "The DART mission is NASA's demonstration of kinetic impactor technology, impacting an asteroid to adjust its speed and path. DART was the first-ever space mission to demonstrate asteroid deflection by kinetic impactor. It impacted the moonlet Dimorphos on September 26, 2022. || ",
            "hits": 283
        },
        {
            "id": 14055,
            "url": "https://svs.gsfc.nasa.gov/14055/",
            "result_type": "Produced Video",
            "release_date": "2021-12-20T22:00:00-05:00",
            "title": "Parker Solar Probe's WISPR Images Inside The Sun's Atmosphere",
            "description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. As Parker Solar Probe flew through the corona, its WISPR instrument captured images.The Wide-Field Imager for Parker Solar Probe (WISPR) is the only imaging instrument aboard the spacecraft. WISPR looks at the large-scale structure of the corona and solar wind before the spacecraft flies through it. About the size of a shoebox, WISPR takes images from afar of structures like coronal mass ejections, or CMEs, jets and other ejecta from the Sun. These structures travel out from the Sun and eventually overtake the spacecraft, where the spacecraft’s other instruments take in-situ measurements. WISPR helps link what’s happening in the large-scale coronal structure to the detailed physical measurements being captured directly in the near-Sun environment.To image the solar atmosphere, WISPR uses the heat shield to block most of the Sun’s light, which would otherwise obscure the much fainter corona. Specially designed baffles and occulters reflect and absorb the residual stray light that has been reflected or diffracted off the edge of the heat shield or other parts of the spacecraft.WISPR uses two cameras with radiation-hardened Active Pixel Sensor CMOS detectors. These detectors are used in place of traditional CCDs because they are lighter and use less power. They are also less susceptible to effects of radiation damage from cosmic rays and other high-energy particles, which are a big concern close to the Sun. The camera’s lenses are made of a radiation hard BK7, a common type of glass used for space telescopes, which is also sufficiently hardened against the impacts of dust.WISPR was designed and developed by the Solar and Heliophysics Physics Branch at the Naval Research Laboratory in Washington, D.C. (principal investigator Russell Howard), which will also develop the observing program. || ",
            "hits": 438
        },
        {
            "id": 4883,
            "url": "https://svs.gsfc.nasa.gov/4883/",
            "result_type": "Visualization",
            "release_date": "2021-02-08T09:00:00-05:00",
            "title": "Apollo 14 Hike To Cone Crater",
            "description": "Full Video with Narration: This video describes the hike toward Cone crater by Apollo 14 astronauts Al Shepard and Ed Mitchell, using a visualization created from Lunar Reconnaissance Orbiter data.Music provided by Universal Production Music: “Taking Flight” – Ben Beiny.Watch this video on the NASA Goddard YouTube channel. || 4883_HikeThumbnail1.jpg (1920x1080) [474.2 KB] || 4883_HikeThumbnail2.jpg (1920x1080) [565.1 KB] || 4883_HikeThumbnail1_print.jpg (1024x576) [161.9 KB] || 4883_Apollo14HikeCone_YouTubeHD.webm (1920x1080) [18.4 MB] || 4883_Apollo14HikeCone_FacebookHD.mp4 (1920x1080) [152.1 MB] || 4883_Apollo14HikeCone_YouTubeHD.mp4 (1920x1080) [202.4 MB] || 4883_Apollo14HikeCone_CAPTIONS.en_US.srt [2.4 KB] || 4883_Apollo14HikeCone_CAPTIONS.en_US.vtt [2.3 KB] || 4883_Apollo14HikeCone_MASTER.mov (1920x1080) [3.1 GB] || ",
            "hits": 356
        },
        {
            "id": 13651,
            "url": "https://svs.gsfc.nasa.gov/13651/",
            "result_type": "Produced Video",
            "release_date": "2020-08-03T11:00:00-04:00",
            "title": "Studying Trojan Asteroids with Lucy",
            "description": "This video highlights the Lucy mission's four main science objectives, and the instruments aboard the spacecraft that will be utilized for the data collection.Music provided by Universal Production Music: \"Feels Good\" - Wally Gagel & Xandy Barry [ASCAP]Watch this video on the NASA Goddard YouTube channel. || LucySciObjThumbnail1_print.jpg (1024x576) [93.0 KB] || LucySciObjThumbnail1_searchweb.png (320x180) [60.4 KB] || LucySciObjThumbnail1_thm.png (80x40) [6.8 KB] || 13651_StudyingAsteroidsLucy_YouTubeHD.mp4 (1920x1080) [128.5 MB] || 13651_StudyingAsteroidsLucy_FacebookHD.mp4 (1920x1080) [101.2 MB] || 13651_StudyingAsteroidsLucy_MASTER.mov (1920x1080) [813.8 MB] || LucySciObjThumbnail1.tif (1920x1080) [7.9 MB] || 13651_StudyingAsteroidsLucy_YouTubeHD.webm (1920x1080) [9.2 MB] || 13651_StudyingAsteroidsLucy.en_US.srt [1.8 KB] || 13651_StudyingAsteroidsLucy.en_US.vtt [1.8 KB] || ",
            "hits": 82
        },
        {
            "id": 13578,
            "url": "https://svs.gsfc.nasa.gov/13578/",
            "result_type": "Produced Video",
            "release_date": "2020-04-13T11:00:00-04:00",
            "title": "NASA Missions Study a Nova's Shock Waves",
            "description": "NASA’s Fermi and NuSTAR space telescopes, together with another satellite named BRITE-Toronto, are providing new insights into a nova explosion that erupted in 2018. Detailed measurements of bright flares in the explosion clearly show that shock waves power most of the nova's visible light.  Credit: NASA’s Goddard Space Flight CenterMusic: \"Scientist\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || novastill01.jpg (3840x2160) [1.1 MB] || novastill01_searchweb.png (320x180) [76.8 KB] || novastill01_thm.png (80x40) [6.7 KB] || 13578_Nova_Carinae_Best.webm (1920x1080) [13.8 MB] || novastill01.tif (3840x2160) [31.7 MB] || 13578_Nova_Carinae_SRT_Captions.en_US.srt [2.2 KB] || 13578_Nova_Carinae_SRT_Captions.en_US.vtt [2.2 KB] || 13578_Nova_Carinae_Best.mp4 (1920x1080) [319.4 MB] || 13578_Nova_Carinae_Good.mp4 (1920x1080) [129.0 MB] || 13578_Nova_Carinae_ProRes_1920x1080_2997.mov (1920x1080) [1.4 GB] || ",
            "hits": 110
        },
        {
            "id": 4733,
            "url": "https://svs.gsfc.nasa.gov/4733/",
            "result_type": "Visualization",
            "release_date": "2019-04-04T00:00:00-04:00",
            "title": "Hyperwall: Scouting the Apollo 11 Landing Site",
            "description": "This sequence of images from Apollo 10 looks west across southern Mare Tranquillitatis. The Apollo 11 landing site is circled in green. The bright crater at about 7 o'clock within the circle is West crater. Black and white, 70mm magazine R, AS10-31-4607 to 11. || apollo10_as10-31-4607_print.jpg (1024x345) [81.6 KB] || apollo10_as10-31-4607_searchweb.png (320x180) [47.4 KB] || apollo10_as10-31-4607_thm.png (80x40) [3.9 KB] || apollo10_as10-31-4607.tif (9600x3240) [13.8 MB] || apollo-10-photo-sequence-of-apollo-11-site.hwshow [237 bytes] || ",
            "hits": 390
        },
        {
            "id": 13035,
            "url": "https://svs.gsfc.nasa.gov/13035/",
            "result_type": "Produced Video",
            "release_date": "2018-08-08T16:00:00-04:00",
            "title": "Parker Solar Probe Instruments",
            "description": "SWEAPThe Solar Wind Electrons Alphas and Protons investigation, or SWEAP, gathers observations using two complementary instruments: the Solar Probe Cup, or SPC, and the Solar Probe Analyzers, or SPAN. The instruments count the most abundant particles in the solar wind — electrons, protons and helium ions — and measure such properties as velocity, density, and temperature to improve our understanding of the solar wind and coronal plasma. SWEAP was built mainly at the Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, and at the Space Sciences Laboratory at the University of California, Berkeley. The institutions jointly operate the instrument. The principal investigator is Justin Kasper from the University of Michigan. || SWEAP.00001_print.jpg (1024x581) [151.9 KB] || SWEAP_thumb.png (2560x1448) [4.7 MB] || SWEAP.00001_searchweb.png (320x180) [86.1 KB] || SWEAP.00001_web.png (320x181) [86.8 KB] || SWEAP.00001_thm.png (80x40) [5.6 KB] || SWEAP.webm (1902x1080) [21.8 MB] || SWEAP.mp4 (1902x1080) [195.4 MB] || SWEAP.en_US.srt [3.8 KB] || SWEAP.en_US.vtt [3.8 KB] || ",
            "hits": 415
        },
        {
            "id": 30970,
            "url": "https://svs.gsfc.nasa.gov/30970/",
            "result_type": "Hyperwall Visual",
            "release_date": "2018-06-25T10:00:00-04:00",
            "title": "Kepler Supernova Remnant",
            "description": "This animation shows the remnant of Kepler's Supernova, shown first in infrared, then visible, then low energy X-ray, then high-energy X-ray emission and finally in combination. || STScI-H-KeplerSNR_1x-1920x1080.00001_print.jpg (1024x576) [18.4 KB] || STScI-H-KeplerSNR_1x-1920x1080.00001_searchweb.png (320x180) [15.9 KB] || STScI-H-KeplerSNR_1x-1920x1080.00001_thm.png (80x40) [2.1 KB] || STScI-H-KeplerSNR_1x-1280x720.mp4 (1280x720) [1.8 MB] || STScI-H-KeplerSNR_1x-1920x1080.mp4 (1920x1080) [3.1 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-KeplerSNR_1x-1920x1080.webm (1920x1080) [6.4 MB] || STScI-H-KeplerSNR_1x-640x360.mp4 (640x360) [708.9 KB] || STScI-H-KeplerSNR_1x-3840x2160.mp4 (3840x2160) [3.8 MB] || STScI-H-KeplerSNR_1x-H265-3840x2160.mp4 (3840x2160) [2.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ",
            "hits": 124
        },
        {
            "id": 30956,
            "url": "https://svs.gsfc.nasa.gov/30956/",
            "result_type": "Hyperwall Visual",
            "release_date": "2018-05-24T12:00:00-04:00",
            "title": "The Red Bubble: Supernova Remnant SNR 0509-67.5",
            "description": "The nebula SNR 0509-67.5, nicknamed the \"Red Bubble\", is the result of a supernova explosion of a star. || red_bubble-sample_frame-1920x1080.png (1920x1080) [971.0 KB] || red_bubble-sample_frame-1920x1080_print.jpg (1024x576) [114.5 KB] || red_bubble-sample_frame-1920x1080_searchweb.png (320x180) [62.8 KB] || red_bubble-sample_frame-1920x1080_thm.png (80x40) [5.6 KB] || red_bubble-1920x1080.webm (1920x1080) [23.3 MB] || red_bubble-1920x1080.wmv (1920x1080) [23.7 MB] || red_bubble-1920x1080.m4v (1920x1080) [23.3 MB] || red_bubble-1920x1080p30.mov (1920x1080) [109.6 MB] || red_bubble-3840x2160p30.mp4 (3840x2160) [142.8 MB] || the-red-bubble-supernova-remnant-snr-0509-675-4k.hwshow [316 bytes] || the-red-bubble-supernova-remnant-snr-0509-675-hd.hwshow [316 bytes] || ",
            "hits": 91
        },
        {
            "id": 30951,
            "url": "https://svs.gsfc.nasa.gov/30951/",
            "result_type": "Hyperwall Visual",
            "release_date": "2018-05-16T10:00:00-04:00",
            "title": "Supernova Remnant Cassiopeia A from Hubble",
            "description": "The nebula known as Cassiopeia A is composed of tattered remains of a star that exploded more than 300 years ago. || cas_a_2004_12-hst-10252x7379_print.jpg (1024x737) [249.8 KB] || cas_a_2004_12-hst-10252x7379_searchweb.png (320x180) [100.4 KB] || cas_a_2004_12-hst-10252x7379_thm.png (80x40) [8.7 KB] || cas_a_2004_12-hst-10252x7379.png (10252x7379) [122.0 MB] || supernova-remnant-cassiopeia-a-from-hubble.hwshow [238 bytes] || ",
            "hits": 146
        },
        {
            "id": 12927,
            "url": "https://svs.gsfc.nasa.gov/12927/",
            "result_type": "Produced Video",
            "release_date": "2018-04-16T12:00:00-04:00",
            "title": "Looking at the Corona with WISPR on Parker Solar Probe",
            "description": "The Wide-Field Imager for Solar Probe, or WISPR, is aboard NASA’s Parker Solar Probe to take images of the solar corona (the Sun’s atmosphere)  and inner heliosphere. WISPR’s telescopes will provide white-light images of the solar wind, shocks, solar ejecta and other structures as they approach and pass the spacecraft. Parker Solar Probe is scheduled for launch in July 2018. It will be the first spacecraft ever to fly through the solar corona to investigate the evolution of the solar wind and heating of the solar corona. WISPR does not look directly at the Sun. Its very wide field-of-view extends from 13° away from the center of the Sun to 108° from the Sun. || ",
            "hits": 86
        },
        {
            "id": 4505,
            "url": "https://svs.gsfc.nasa.gov/4505/",
            "result_type": "Visualization",
            "release_date": "2016-10-13T00:01:00-04:00",
            "title": "Gardening Rates on the Moon",
            "description": "After simulating the distant view of a new impact, the camera zooms up to the surface to show actual before/after images of a new 12-meter crater taken by the Lunar Reconnaissance Orbiter narrow-angle camera. (The impact that formed this crater wasn't seen from Earth, but a different one was.) || new_crater.0900_print.jpg (1024x576) [183.2 KB] || new_crater.0900_searchweb.png (320x180) [66.2 KB] || new_crater.0900_thm.png (80x40) [3.5 KB] || new_crater_1080p30.mp4 (1920x1080) [17.9 MB] || new_crater_720p30.mp4 (1280x720) [9.1 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || new_crater_720p30.webm (1280x720) [2.9 MB] || new_crater_360p30.mp4 (640x360) [3.0 MB] || new_crater_4505.key [19.1 MB] || new_crater_4505.pptx [18.8 MB] || gardening-moon-mp4.hwshow [204 bytes] || ",
            "hits": 224
        },
        {
            "id": 4242,
            "url": "https://svs.gsfc.nasa.gov/4242/",
            "result_type": "Visualization",
            "release_date": "2015-03-17T14:00:00-04:00",
            "title": "March 17, 2013 Lunar Impact Forms a New Crater",
            "description": "Artist's conception of the March 17, 2013 lunar impact as seen from near the impact site in Mare Imbrium.This video is also available on our YouTube channel. || impactb.0172_print.jpg (1024x576) [43.7 KB] || impactb.0172_searchweb.png (320x180) [39.8 KB] || impactb.0172_thm.png (80x40) [3.6 KB] || from_moon_720p30.webmhd.webm (960x540) [249.9 KB] || from_moon_1080p30.mp4 (1920x1080) [629.5 KB] || from_moon_720p30.mp4 (1280x720) [298.3 KB] || from_moon (1920x1080) [0 Item(s)] || from_moon_360p30.mp4 (640x360) [100.4 KB] || from_moon_4242.key [2.8 MB] || from_moon_4242.pptx [390.9 KB] || ",
            "hits": 256
        },
        {
            "id": 4185,
            "url": "https://svs.gsfc.nasa.gov/4185/",
            "result_type": "Visualization",
            "release_date": "2014-07-18T09:00:00-04:00",
            "title": "A New Look at the Apollo 11 Landing Site",
            "description": "Apollo 11 landed on the Moon on July 20th, 1969, a little after 4:00 in the afternoon Eastern Daylight Time. The Lunar Module, nicknamed Eagle and flown by Neil Armstrong and Edwin \"Buzz\" Aldrin, touched down near the southern rim of the Sea of Tranquility, one of the large, dark basins that contribute to the Man in the Moon visible from Earth. Armstrong and Aldrin spent about two hours outside the LM setting up experiments and collecting samples. At one point, Armstrong ventured east of the LM to examine a small crater, dubbed Little West, that he'd flown over just before landing.The trails of disturbed regolith created by the astronauts' boots are still clearly visible in photographs of the landing site taken by the Lunar Reconnaissance Orbiter (LRO) narrow-angle camera (LROC) more than four decades later.LROC imagery makes it possible to visit the landing site in a whole new way by flying around a three-dimensional model of the site. LROC scientists created the digital elevation model using a stereo pair of images. Each image in the pair shows the site from a slightly different angle, allowing sophisticated software to infer the shape of the terrain, similar to the way that left and right eye views are combined in the brain to produce the perception of depth.The animator draped an LROC photograph over the terrain model. He also added a 3D model of the LM descent stage—the real LM in the photograph looks oddly flat when viewed at an oblique angle.Although the area around the site is relatively flat by lunar standards, West Crater (the big brother of the crater visited by Armstrong) appears in dramatic relief near the eastern edge of the terrain model. Ejecta from West comprises the boulders that Armstrong had to avoid as he searched for a safe landing site.Apollo 11 was the first of six increasingly ambitious crewed lunar landings. The exploration of the lunar surface by the Apollo astronauts, when combined with the wealth of remote sensing data now being returned by LRO, continues to inform our understanding of our nearest neighbor in space. || ",
            "hits": 2593
        },
        {
            "id": 4220,
            "url": "https://svs.gsfc.nasa.gov/4220/",
            "result_type": "Visualization",
            "release_date": "2014-06-18T00:00:00-04:00",
            "title": "Hyperwall: Tycho Central Peak",
            "description": "This image set is formatted for NASA's hyperwall, a tiled display with a combined resolution of up to 9600 x 3240.On June 10, 2011, Lunar Reconnaissance Orbiter (LRO) slewed 65° to the west, allowing its narrow-angle camera (the LROC NAC) to capture this dramatic sunrise view of the mountains at the center of Tycho crater. It's not hard to see why this image was the winner of the Moon as Art contest.A popular target of amateur astronomers, Tycho is located at 43.3°S, 11.4°W, and is about 85 kilometers (55 miles) wide. A system of bright ejecta rays radiating from the crater is easily visible in binoculars and small telescopes during Full Moon. The crater's features are so steep and sharp because it's only about 110 million years old, quite young by lunar standards. || ",
            "hits": 145
        },
        {
            "id": 11494,
            "url": "https://svs.gsfc.nasa.gov/11494/",
            "result_type": "Produced Video",
            "release_date": "2014-03-24T06:00:00-04:00",
            "title": "Jim Garvin's Top \"Pics\" - LROC Images",
            "description": "In this video series, NASA Scientist Jim Garvin highlights his favorite pictures taken throughout the solar system. This episode focuses on images taken by LROC – the Lunar Reconnaissance Orbiter Camera. Jim explains which pictures made his “top 5” list. || ",
            "hits": 117
        },
        {
            "id": 3731,
            "url": "https://svs.gsfc.nasa.gov/3731/",
            "result_type": "Visualization",
            "release_date": "2010-06-21T00:00:00-04:00",
            "title": "LOLA: Lunar Topography in Natural Color",
            "description": "This animation is a brief tour of several prominent features of the Moon's terrain: Tycho crater, the south pole, and the South Pole-Aitken basin. It is match-moved to a companion piece showing the terrain elevations in false color.This is an update of animation 3594, which was produced before the launch of Lunar Reconnaissance Orbiter. Except for the Tycho crater inset, the elevation map in this updated version is based entirely on early results of the Lunar Orbiter Laser Altimeter onboard LRO.The surface appearance is derived from photographs taken by the Clementine spacecraft. Although it shows the visible surface in natural color, this animation does not depict realistic sunlight and shadows. This is especially significant near the poles, where certain parts of the terrain can be in permanent shadow and would never be fully visible in the manner depicted here. || ",
            "hits": 241
        },
        {
            "id": 3727,
            "url": "https://svs.gsfc.nasa.gov/3727/",
            "result_type": "Visualization",
            "release_date": "2010-06-11T00:00:00-04:00",
            "title": "LOLA Lunar Topography in False Color",
            "description": "This animation is a brief tour of several prominent features of the Moon's terrain: Tycho crater, the south pole, and the South Pole-Aitken basin. The height of the terrain is color-coded, with blues and greens representing low altitudes and reds representing high altitudes. The view is match-moved to a companion piece showing the Moon in natural colors.This is an update of animation 3582, which was produced before the launch of Lunar Reconnaissance Orbiter. Except for the Tycho crater inset, the elevation map in this updated version is based entirely on early results of the Lunar Orbiter Laser Altimeter onboard LRO. These results already represent a substantial improvement in our knowledge of the Moon's topography. || ",
            "hits": 300
        },
        {
            "id": 3634,
            "url": "https://svs.gsfc.nasa.gov/3634/",
            "result_type": "Visualization",
            "release_date": "2009-09-17T12:00:00-04:00",
            "title": "Shackleton's Rim Through the Eyes of LRO/LROC",
            "description": "During the Lunar Reconnaissance Oribiter's (LRO) Commissioning Phase, the high resolution Narrow Angle Camera (NAC) on the LRO Camera (LROC) instrument captured this 0.8-meter per pixel scale (angular resolution) two-image mosaic of Shackleton Crater on the moon's south pole. Many more images of this area will be obtained by the NAC over the coming months as the lunar south pole emerges from the shadows of winter. At meter scales, the geology of this region reminds us that the polar regions of the Moon are still waiting to be explored. The rim of Shackleton crater is a prime candidate for future human exploration due to its proximity to permanently shadowed regions and nearby peaks that are illuminated for much of the year.Last year, Japan's Selene and India's Chandrayaan spacecraft gave us our first high resolution look at the lunar south pole, which includes Shackleton crater. For its size, Shackleton has an exceptionally deep and rugged interior. Usually craters fill in with time as their walls slump and material from afar is thrown in by distant impacts. Much of Shackleton's rim appears rounded and is peppered with smaller craters, indications of a relatively ancient age. Right now it is not clear if Shackleton crater is relatively old or young. This NAC image reveals a shelf on the southeast flank of the crater that is more than two kilometers across and perfectly suitable for a future landing. The extreme Sun angle exaggerates the apparent roughness, however if you look closely at this scale any area that is between small craters could be good candidates for a potential landing site. || ",
            "hits": 95
        },
        {
            "id": 10447,
            "url": "https://svs.gsfc.nasa.gov/10447/",
            "result_type": "Produced Video",
            "release_date": "2009-07-07T00:00:00-04:00",
            "title": "Flyover of the First Images from the Lunar Reconnaissance Orbiter Camera",
            "description": "A starkly beautiful region a few kilometers east of Hell E crater, which is located on the floor of the ancient Imbrian-aged Deslandres impact structure in the lunar highlands south of Mare Nubium. Numerous small, secondary craters can be identified, including several small crater chains. Also identifiable are distinctive lineations made readily apparent by the extreme lighting, representing ejecta from a nearby impact. The NAC image shown here has not been calibrated and the pixel values were stretched to enhance contrast. Image width is 3.5 km x 70 km; north is down. || ",
            "hits": 60
        },
        {
            "id": 3582,
            "url": "https://svs.gsfc.nasa.gov/3582/",
            "result_type": "Visualization",
            "release_date": "2009-04-17T00:00:00-04:00",
            "title": "Lunar Topography in False Color",
            "description": "An updated version of this animation is available here.This animation is a brief tour of several prominent features of the Moon's terrain: Tycho crater, the south pole, and the South Pole-Aitken basin. The height of the terrain is color-coded, with blues and greens representing low altitudes and reds representing high altitudes. The view is match-moved to a companion piece showing the Moon in natural colors.The elevation map comprises low-resolution data from a number of sources, including the Clementine and JAXA/SELENE spacecraft, combined with high-resolution insets for Tycho and the region near the south pole. One of the goals of the Lunar Reconnaissance Orbiter mission is the creation of a high-resolution elevation map of the entire surface of the Moon. || ",
            "hits": 257
        },
        {
            "id": 3594,
            "url": "https://svs.gsfc.nasa.gov/3594/",
            "result_type": "Visualization",
            "release_date": "2009-04-17T00:00:00-04:00",
            "title": "Lunar Topography in Natural Color",
            "description": "An updated version of this animation is available here.This animation is a brief tour of several prominent features of the Moon's terrain: Tycho crater, the south pole, and the South Pole-Aitken basin. It is match-moved to a companion piece showing the terrain elevations in false color.The surface appearance is derived from photographs taken by the Clementine spacecraft. Although it shows the visible surface in natural color, this animation does not depict realistic sunlight and shadows. This is especially significant near the poles, where certain parts of the terrain can be in permanent shadow and would never be fully visible in the manner depicted here. || ",
            "hits": 252
        },
        {
            "id": 20067,
            "url": "https://svs.gsfc.nasa.gov/20067/",
            "result_type": "Animation",
            "release_date": "2003-03-20T12:00:00-05:00",
            "title": "Cannibal CME",
            "description": "This sequence of images is from a computer animation illustrating an artist's concept of Coronal Mass Ejection (CME) cannibalism. Coronal Mass Ejections (CMEs) are clouds of electrified, magnetic gas weighing billions of tons ejected from the Sun and hurled into space with speeds ranging from 12 to 1,250 miles per second (about 20 to 2,000 kilometers per second). The first CME blasts from the right side of the sun (bright, white area), and as it expands into space, it becomes fainter. A second CME erupts from near the same region on the Sun as the first CME, appearing as another bright burst on the right side of the Sun. The second CME is moving faster than the first, and it overtakes and assimilates the first CME in frames four through six. Solar researchers believe cannibal CMEs may be the source of 'complex ejecta' CME clouds; those with a larger and more complex structure than typical CMEs. These traits cause complex ejecta CMEs to trigger protracted magnetic storms when they envelop the Earth. || ",
            "hits": 156
        },
        {
            "id": 39,
            "url": "https://svs.gsfc.nasa.gov/39/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Density",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 77
        },
        {
            "id": 40,
            "url": "https://svs.gsfc.nasa.gov/40/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Hydrogen Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 93
        },
        {
            "id": 41,
            "url": "https://svs.gsfc.nasa.gov/41/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Hydrogen",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 43
        },
        {
            "id": 42,
            "url": "https://svs.gsfc.nasa.gov/42/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Helium Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 45
        },
        {
            "id": 43,
            "url": "https://svs.gsfc.nasa.gov/43/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Helium",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosionto maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 41
        },
        {
            "id": 44,
            "url": "https://svs.gsfc.nasa.gov/44/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Oxygen Mass Fraction",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 15
        },
        {
            "id": 45,
            "url": "https://svs.gsfc.nasa.gov/45/",
            "result_type": "Visualization",
            "release_date": "1994-02-12T12:00:00-05:00",
            "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Oxygen",
            "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ",
            "hits": 52
        }
    ]
}