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    "results": [
        {
            "id": 5569,
            "url": "https://svs.gsfc.nasa.gov/5569/",
            "result_type": "Visualization",
            "release_date": "2025-07-11T09:30:59-04:00",
            "title": "Texas Hill Country Hit by Powerful Floods",
            "description": "GPM passed over the Texas storm on July 4th, 11am CT.",
            "hits": 65
        },
        {
            "id": 14631,
            "url": "https://svs.gsfc.nasa.gov/14631/",
            "result_type": "Produced Video",
            "release_date": "2024-07-22T11:00:00-04:00",
            "title": "Model Behavior: Visualizing Global CO2",
            "description": "Universal Production Music: Prismatic by David Stephen Goldsmith [ PRS ]Complete transcript available. || 14631_DYAMONDThumbnailHorz.jpg (1280x720) [291.1 KB] || 14631_DYAMONDThumbnailHorz_print.jpg (1024x576) [222.2 KB] || 14631_DYAMONDThumbnailHorz_searchweb.png (320x180) [91.4 KB] || 14631_DYAMONDThumbnailHorz_thm.png (80x40) [7.1 KB] || 14631_dyamondhorz_US.en.en_US.srt [2.3 KB] || 14631_dyamondhorz_US.en.en_US.vtt [2.2 KB] || 14631_DYAMOND_Horz.webm (3840x2160) [32.4 MB] || 14631_DYAMOND_Horz.mp4 (3840x2160) [267.6 MB] || ",
            "hits": 266
        },
        {
            "id": 5305,
            "url": "https://svs.gsfc.nasa.gov/5305/",
            "result_type": "Visualization",
            "release_date": "2024-07-02T08:00:00-04:00",
            "title": "2023 Atlantic Hurricane Season",
            "description": "The 2023 Atlantic Hurricane Season from June 1st through October 31st. The colors over the ocean are Sea Surface Temperatures where reds are high temperatures and blues are low. The colors underneath the clouds are precipitation measurements, where red is high and greens are low. Each hurricane name tracks with it's corresponding storm and leaves behind category designations (TD=Tropical Depression; TS=Tropical Storm; and 1 through 5 are hurricane strengths) as each storm increases and decreases in strength. || hurr2023_v34_ALL_2024-06-26_1103.00001_print.jpg (1024x576) [234.5 KB] || hurr2023_v34_ALL_2024-06-26_1103.00001_searchweb.png (320x180) [101.0 KB] || hurr2023_v34_ALL_2024-06-26_1103.00001_thm.png (80x40) [6.8 KB] || hurr2023_v34_ALL_2024-06-26_1103_1080p30.webm (1920x1080) [44.7 MB] || All_Data_in_HD [0 Item(s)] || hurr2023_v34_ALL_2024-06-26_1103_1080p30.mp4 (1920x1080) [739.1 MB] || ALL_Data_in_UHD [0 Item(s)] || hurr2023_v34_ALL_4k.mp4 (3840x2160) [2.3 GB] || ",
            "hits": 129
        },
        {
            "id": 14536,
            "url": "https://svs.gsfc.nasa.gov/14536/",
            "result_type": "Produced Video",
            "release_date": "2024-02-26T14:45:00-05:00",
            "title": "NASA's SDO Captures a February Solar Flare Triple Play",
            "description": "The Solar Dynamics Observatory (SDO) spotted three X-class flares on the Sun between February 21 and 22, 2024.  Watch this video to see what those events looked like in several wavelengths of extreme ultraviolet light that SDO captures. The video opens with quick shots of the three flares in different wavelength blends.  The first is a blend of 131 and 171-angstrom-light imagery, the second is 171 and 304, and the last is 171 and 1600.  Each wavelength highlights different temperature plasma and reveals different layers and features of the Sun. 131 angstrom light shows both the extremely hot plasma of flares (6-10 million Kelvin) and cooler plasma (400,000 Kelvin).  Credit: NASA's Goddard Space Flight Center/SDOMusic: \"Serene Reverie\" from the album Reflections.  Written and produced by Lars Leonhard.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || February_Triple_Play_Still_print.jpg (1024x576) [166.0 KB] || February_Triple_Play_Still.jpg (3840x2160) [2.1 MB] || February_Triple_Play_Still_searchweb.png (320x180) [100.7 KB] || February_Triple_Play_Still_thm.png (80x40) [8.0 KB] || 14536_FebruaryXFlareTriplePlay_1080.webm (1920x1080) [26.0 MB] || Flare_Triple_Play_Captions.en_US.srt [811 bytes] || Flare_Triple_Play_Captions.en_US.vtt [772 bytes] || 14536_FebruaryXFlareTriplePlay_1080.mp4 (1920x1080) [405.7 MB] || 14536_FebruaryXFlareTriplePlay_1080_small.mp4 (1920x1080) [166.7 MB] || 14536_FebruaryXFlareTriplePlay_ProRes_3840x2160.mov (3840x2160) [14.2 GB] || 14536_FebruaryXFlareTriplePlay_4k_25mbps.mp4 (3840x2160) [670.9 MB] || 14536_FebruaryXFlareTriplePlay_4k_50mbps.mp4 (3840x2160) [1.3 GB] || ",
            "hits": 190
        },
        {
            "id": 14531,
            "url": "https://svs.gsfc.nasa.gov/14531/",
            "result_type": "Produced Video",
            "release_date": "2024-02-20T10:00:00-05:00",
            "title": "February 16, 2024 X2.5 Solar Flare",
            "description": "NASA’s Solar Dynamics Observatory captured these images of a solar flare – as seen in the bright flash on the right of each image – on Feb. 16, 2024. The images show three subsets of extreme ultraviolet light that highlight the extremely hot material in flares and which are colorized in teal, gold, and red. Credit: NASA/SDO || Feb_16_Flare_Video_multi_still.jpg (1920x1080) [389.3 KB] || Feb_16_Flare_Video_multi_still_searchweb.png (320x180) [85.5 KB] || Feb_16_Flare_Video_multi_still_thm.png (80x40) [7.1 KB] || Feb_16_Flare_Video_multi.mp4 (1920x1080) [53.9 MB] || Feb_16_Flare_Video_multi.mov (1920x1080) [379.3 MB] || ",
            "hits": 92
        },
        {
            "id": 14434,
            "url": "https://svs.gsfc.nasa.gov/14434/",
            "result_type": "Produced Video",
            "release_date": "2023-11-28T09:20:00-05:00",
            "title": "NASA’s Fermi Mission Finds 300 Gamma-Ray Pulsars",
            "description": "This visualization shows 294 gamma-ray pulsars, first plotted on an image of the entire starry sky as seen from Earth and then transitioning to a view from above our galaxy. The symbols show different types of pulsars. Young pulsars blink in real time except for the Crab, which pulses slower because its rate is only slightly lower than the video frame rate. Millisecond pulsars remain steady, pulsing too quickly to see. The Crab, Vela, and Geminga were among the 11 gamma-ray pulsars known before Fermi launched. Other notable objects are also highlighted. Distances are shown in light-years (abbreviated ly).Credit: NASA’s Goddard Space Flight CenterMusic: \"Fascination\" from Universal Production MusicWatch this video on the NASA.gov Video YouTube channel.Complete transcript available. || Pulsar_Still.jpg (3840x2160) [3.5 MB] || Pulsar_Still_searchweb.png (320x180) [105.5 KB] || Pulsar_Still_thm.png (80x40) [7.0 KB] || 14434_Fermi_Pulsar_Locations_1080.mp4 (1920x1080) [93.9 MB] || 14434_Fermi_Pulsar_Locations_1080.webm (1920x1080) [10.0 MB] || Pulsar_Captions.en_US.srt [46 bytes] || Pulsar_Captions.en_US.vtt [56 bytes] || 14434_Fermi_Pulsar_Locations_4k_Good.mp4 (3840x2160) [112.8 MB] || 14434_Fermi_Pulsar_Locations_4k_Best.mp4 (3840x2160) [689.2 MB] || 14434_Fermi_Pulsar_Locations_ProRes_3840x2160_2997.mov (3840x2160) [4.5 GB] || ",
            "hits": 382
        },
        {
            "id": 10662,
            "url": "https://svs.gsfc.nasa.gov/10662/",
            "result_type": "Produced Video",
            "release_date": "2021-04-14T00:00:00-04:00",
            "title": "Webb Science Simulations: Planetary Systems and Origins of Life",
            "description": "Supercomputer simulations of planeratry evolution. Part 1: Turbulent Molecular Cloud Nebula with Protostellar ObjectsThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk and Michael Norman to visualize a computational data set of a turbulent molecular cloud nebula forming protostellar objects and accretion disks approximately 100 AU in diameter, on the order of the size of our solar system. AVL used its Amore software to interpolate and render the Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics. The AMR simulation was developed by Drs. Kritsuk and Norman at the Laboratory for Computational Astrophysics. The AMR simulation generated more than 2 terabytes of data and follows star formation processes in a self-gravitating turbulent molecular cloud with a dynamic range of half-a-million in linear scale, resolving both the large-scale filamentary structure of the molecular cloud (~5 parsec) and accretion disks around emerging young protostellar objects (down to 2 AU).  Part 2: Protoplanetary Disk and Planet FormationThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Dr. Aaron Boley to visualize the 16,000 year evolution of a young, isolated protoplanetary disk which surrounds a newly-formed protostar. The disk forms spiral arms and a dense clump as a result of gravitational collapse. Dr. Aaron Boley developed this computational model to investigate the response of young disks to mass accretion from their surrounding envelopes, including the direct formation of planets and brown dwarfs through gravitational instability.  The main formation mechanism for gas giant planets has been debated within the scientific community for over a decade. One of these theories is 'direct formation through gravitational instability.' If the self-gravity of the gas overwhelms the disk's thermal pressure and the stabilizing effect of differential rotation, the gas closest to the protostar rotates faster than gas farther away. In this scenario, regions of the gaseous disk collapse and form a planet directly. The study, presented in Boley (2009), explores whether mass accretion in the outer regions of disks can lead to such disk fragmentation. The simulations show that clumps can form in situ at large disk radii. If the clumps survive, they can become gas giants on wide orbits, e.g., Fomalhaut b, or even more massive objects called brown dwarfs. Whether a disk forms planets at large radii and, if so, the number of planets that form, depend on how much of the envelope mass is distributed at large distances from the protostar.  The results of the simulations suggest that there are two modes of gas giant planet formation. The first mode occurs early in the disk's lifetime, at large radii, and through the disk instability mechanism. After the main accretion phase is over, gas giants can form in the inner disk, over a period of a million years, through the core accretion mechanism, which researchers are addressing in other studies.Thanks to R. H. Durisen, L. Mayer, and G. Lake for comments and discussions relating to this research. This study was supported in part by the University of Zurich, Institute for Theoretical Physics, and by a Swiss Federal Grant. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.AVL at NCSA, University of Illinois. || ",
            "hits": 605
        },
        {
            "id": 13493,
            "url": "https://svs.gsfc.nasa.gov/13493/",
            "result_type": "Produced Video",
            "release_date": "2019-12-10T11:00:00-05:00",
            "title": "Terra Satellite 20-Year Anniversary Instruments and Applications",
            "description": "Music: “Blackbird” by Magnum Opus [ASCAP]; Atmosphere Music Ltd [PRS]; Volta Music; Universal Production Music || 13493_Terra_Applications_20Anniversary_FINAL.02146_print.jpg (1024x576) [230.0 KB] || 13493_Terra_Applications_20Anniversary_FINAL.02146_searchweb.png (320x180) [132.3 KB] || 13493_Terra_Applications_20Anniversary_FINAL.02146_thm.png (80x40) [8.0 KB] || 13493_Terra_Applications_20Anniversary_FINAL.mov (1920x1080) [4.1 GB] || 13493_Terra_Applications_20Anniversary_FINAL_VX-309499.webm (960x540) [73.2 MB] || 13493_Terra_Applications_20Anniversary_FINAL_VX-309499_lowres.mp4 (1280x720) [51.8 MB] || YOUTUBE_1080_13493_Terra_Applications_20Anniversary_FINAL_VX-309499_youtube_1080.mp4 (1920x1080) [269.9 MB] || YOUTUBE_720_13493_Terra_Applications_20Anniversary_FINAL_VX-309499_youtube_720.mp4 (1280x720) [272.1 MB] || 13493_Terra_Applications_20Anniversary_FINAL.en_US.srt [2.4 KB] || 13493_Terra_Applications_20Anniversary_FINAL.en_US.vtt [2.4 KB] || ",
            "hits": 42
        },
        {
            "id": 11541,
            "url": "https://svs.gsfc.nasa.gov/11541/",
            "result_type": "Produced Video",
            "release_date": "2014-06-05T00:00:00-04:00",
            "title": "Creating Gas Giants",
            "description": "Ancient civilizations observed Jupiter in the night sky, but humanity still doesn’t completely understand how it and other giant gas planets are born. One theory is that they began as rocky planets that slowly accumulated thick atmospheres and expanded into big gaseous bodies over millions of years. But there might be a faster route. Solar systems grow from protoplanetary disks, a large stew of primordial gases surrounding a massive solar seed called a protostar. Over thousands of years, the protostar’s gravity sucks in material from the disk’s outer reaches. As more gas swirls inward, it’s packed into dense spiral arms. While the protostar will eventually consume the gas closest to it, material farther away may spin off and condense into a Jupiter-like planet. Watch the video to see this process unfold. || ",
            "hits": 104
        },
        {
            "id": 10986,
            "url": "https://svs.gsfc.nasa.gov/10986/",
            "result_type": "Produced Video",
            "release_date": "2012-06-26T00:00:00-04:00",
            "title": "A Star's Spiral",
            "description": "NASA-supported researchers using a Japanese telescope in Hawaii have taken the first clear image of a rare sight: a star surrounded by a spiral-armed disk. Telescope images have shown hints of stars with spiral disks before. The clarity of this new image, however, is allowing researchers to study what causes this kind of spiral. Rings called circumstellar disks—composed of gas, dust and an accumulation of small objects—surround some stars. If the ring contains planets, their gravitational pull could alter its circular form and create the spiral arms. These videos take a closer look at the new image of star SAO 206462 and raise the question of whether orbiting planets, or something else entirely, created this curious shape. || ",
            "hits": 213
        },
        {
            "id": 10847,
            "url": "https://svs.gsfc.nasa.gov/10847/",
            "result_type": "Produced Video",
            "release_date": "2011-10-19T09:30:00-04:00",
            "title": "Spiral Arms Point to Possible Planets in a Star's Dusty Disk",
            "description": "A new image of the disk of gas and dust around a sun-like star is the first to show spiral-arm-like structures. These features may provide clues to the presence of embedded but as-yet-unseen planets.The newly imaged disk surrounds SAO 206462, an 8.7-magnitude star located about 456 light-years away in the constellation Lupus. Astronomers estimate that the system is only about 9 million years old. The gas-rich disk spans some 14 billion miles, which is more than twice the size of Pluto's orbit in our own solar system. The Subaru near-infrared image reveals a pair of spiral features arcing along the outer disk. Theoretical models show that a single embedded planet may produce a spiral arm on each side of a disk. The structures around SAO 206462 do not form a matched pair, suggesting the presence of two unseen worlds, one for each arm. || ",
            "hits": 350
        },
        {
            "id": 10659,
            "url": "https://svs.gsfc.nasa.gov/10659/",
            "result_type": "Produced Video",
            "release_date": "2010-10-28T00:00:00-04:00",
            "title": "JWST Feature - Planetary Evolution",
            "description": "A fully produced video about planetary evolution and how the Webb Telelscope's ability to see inside dense clouds of gas and dust will help us better understand solar system formation and evolution. || ",
            "hits": 517
        }
    ]
}