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    "results": [
        {
            "id": 14704,
            "url": "https://svs.gsfc.nasa.gov/14704/",
            "result_type": "Produced Video",
            "release_date": "2024-10-23T06:00:00-04:00",
            "title": "NASA Interview Opportunity: Star light, star bright, check out the evening sky on your Halloween walk tonight",
            "description": "Scroll down the page to find b-roll for the live shots + a pre-recorded interview with Rebekah HounsellFor more information check out: @NASAUniverse on social media platforms and universe.nasa.gov online || T_CrB_banner_-_ENGLISH.png (1800x720) [1.8 MB] || T_CrB_banner_-_ENGLISH_print.jpg (1024x409) [109.8 KB] || T_CrB_banner_-_ENGLISH_searchweb.png (320x180) [80.0 KB] || T_CrB_banner_-_ENGLISH_thm.png (80x40) [7.0 KB] || ",
            "hits": 67
        },
        {
            "id": 14677,
            "url": "https://svs.gsfc.nasa.gov/14677/",
            "result_type": "Produced Video",
            "release_date": "2024-10-02T10:00:00-04:00",
            "title": "NASA's TESS Spots Record-breaking Stellar Triplets",
            "description": "This artist’s concept illustrates how tightly the three stars in the system called TIC 290061484 orbit each other. If they were placed at the center of our solar system, all the stars’ orbits would be contained a space smaller than Mercury’s orbit around the Sun. The sizes of the triplet stars and the Sun are also to scale.Credit: NASA’s Goddard Space Flight Center || TESS_Triple_system_beauty_scale.jpg (3840x2160) [775.5 KB] || ",
            "hits": 444
        },
        {
            "id": 14133,
            "url": "https://svs.gsfc.nasa.gov/14133/",
            "result_type": "Produced Video",
            "release_date": "2022-04-06T13:00:00-04:00",
            "title": "Concert videos",
            "description": "These videos are designed to accompany live orchestral performances.  For more information and inquiries about their use, please contact Scott Wiessinger at scott.wiessinger@nasa.gov. || ",
            "hits": 49
        },
        {
            "id": 13852,
            "url": "https://svs.gsfc.nasa.gov/13852/",
            "result_type": "Produced Video",
            "release_date": "2021-05-26T10:00:00-04:00",
            "title": "NASA’s Roman Mission to Probe Cosmic Secrets Using Exploding Stars",
            "description": "NASA’s upcoming Nancy Grace Roman Space Telescope will see thousands of exploding stars called supernovae across vast stretches of time and space. Using these observations, astronomers aim to shine a light on several cosmic mysteries, providing a window onto the universe’s distant past and hazy present.Credit: NASA's Goddard Space Flight CenterMusic: \"Relentless Data\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Supernova_IA_1285_print.jpg (1024x576) [53.0 KB] || Supernova_IA_1285.png (3840x2160) [5.0 MB] || Supernova_IA_1285_searchweb.png (320x180) [46.9 KB] || Supernova_IA_1285_thm.png (80x40) [4.6 KB] || 13852_Roman_Standard_Candle_Supernovae_1080_Best.webm (1920x1080) [28.3 MB] || 13852_Roman_Standard_Candle_Supernovae_1080.mp4 (1920x1080) [136.7 MB] || 13852_Roman_Standard_Candle_Supernovae_1080_Best.mp4 (1920x1080) [654.2 MB] || 13852RomanStandardCandleSupernovaeCaptionsFix.en_US.srt [4.7 KB] || 13852RomanStandardCandleSupernovaeCaptionsFix.en_US.vtt [4.7 KB] || 13852_Roman_Standard_Candle_Supernovae_ProRes_1920x1080_2997.mov (1920x1080) [3.2 GB] || ",
            "hits": 119
        },
        {
            "id": 20344,
            "url": "https://svs.gsfc.nasa.gov/20344/",
            "result_type": "Animation",
            "release_date": "2021-05-26T10:00:00-04:00",
            "title": "Type Ia Supernovae Animations",
            "description": "White Dwarf establishing shot. || WDStar_4k_60fps_ProRes.00600_print.jpg (1024x576) [27.4 KB] || WDStar_4k_60fps_ProRes.00600_searchweb.png (320x180) [30.7 KB] || WDStar_4k_60fps_ProRes.00600_thm.png (80x40) [3.2 KB] || WDStar_4k_60fps_h264.mp4 (3840x2160) [37.3 MB] || WDStar_4k (3840x2160) [0 Item(s)] || WDStar_4k_60fps_ProRes.webm (3840x2160) [4.1 MB] || WDStar_4k_60fps_ProRes.mov (3840x2160) [3.0 GB] || ",
            "hits": 386
        },
        {
            "id": 13806,
            "url": "https://svs.gsfc.nasa.gov/13806/",
            "result_type": "Produced Video",
            "release_date": "2021-03-12T11:00:00-05:00",
            "title": "Scientists Build a Detailed Image of U Mon Binary",
            "description": "Two stars orbit each other within an enormous dusty disk in the U Monocerotis system, illustrated here. When the stars are farthest from each other, they funnel material from the disk’s inner edge. At this time, the primary star is slightly obscured by the disk from our perspective. The primary star, a yellow supergiant, expands and contracts. The smaller secondary star is thought to maintain its own disk of material, which likely powers an outflow of gas that emits X-rays.This listing includes Spanish-language and music-free versions.Credit: NASA’s Goddard Space Flight Center/Chris Smith (USRA/GESTAR)Music: \"Moving in Thought\" from Universal Production MusicNote: While this video in its entirety can be shared without permission, its music has been licensed and may not be excised or remixed in other products. || u_mon_full_edit_still.jpg (1920x1080) [707.8 KB] || u_mon_full_edit_still_print.jpg (1024x576) [294.6 KB] || u_mon_full_edit_still_searchweb.png (320x180) [80.8 KB] || u_mon_full_edit_still_web.png (320x180) [80.8 KB] || u_mon_full_edit_still_thm.png (80x40) [6.4 KB] || u_mon_full_edit_w_music_spanish_LQ.mp4 (1920x1080) [47.5 MB] || u_mon_full_edit_HQ.mp4 (1920x1080) [90.3 MB] || u_mon_full_edit_w_music_LQ.mp4 (1920x1080) [47.5 MB] || u_mon_full_edit_w_music_SVS_preview.webm (1280x720) [5.5 MB] || u_mon_full_edit_w_music_spanish_prores.mov (1920x1080) [526.2 MB] || u_mon_full_edit_w_music_spanish_HQ.mp4 (1920x1080) [96.6 MB] || u_mon_full_edit_w_music_prores.mov (1920x1080) [526.5 MB] || u_mon_full_edit_w_music_SVS_preview.mp4 (1280x720) [30.0 MB] || u_mon_full_edit_w_music_HQ.mp4 (1920x1080) [96.6 MB] || u_mon_full_edit_spanish_prores.mov (1920x1080) [488.5 MB] || u_mon_full_edit_prores.mov (1920x1080) [488.8 MB] || u_mon_full_edit_LQ.mp4 (1920x1080) [48.6 MB] || u_mon_full_edit_captions.en_US.vtt [536 bytes] || u_mon_full_edit_captions.en_US.srt [581 bytes] || ",
            "hits": 28
        },
        {
            "id": 13636,
            "url": "https://svs.gsfc.nasa.gov/13636/",
            "result_type": "Produced Video",
            "release_date": "2020-09-30T10:00:00-04:00",
            "title": "Join the Hunt for New Worlds Through Planet Patrol",
            "description": "Want to hunt the skies for uncharted worlds from home? Join Planet Patrol! Watch to learn how you can collaborate with professional astronomers and analyze images from NASA's Transiting Exoplanet Survey Satellite (TESS) on your own. You'll answer questions about each TESS image and help scientists figure out if they contain signals from new worlds or planetary imposters.Credit: NASA's Goddard Space Flight Center/Conceptual Image LabMusic: \"A Wonderful Loaf\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Planet_Patrol_Still-logo_print.jpg (1024x576) [111.4 KB] || Planet_Patrol_Still-logo.jpg (3840x2160) [1.1 MB] || Planet_Patrol_Still-logo_searchweb.png (320x180) [61.9 KB] || Planet_Patrol_Still-logo_thm.png (80x40) [9.8 KB] || 13636_Planet_Patrol_Best_1080.mp4 (1920x1080) [100.9 MB] || 13636_Planet_Patrol_1080.mp4 (1920x1080) [39.6 MB] || 13636_Planet_Patrol_Best_1080.webm (1920x1080) [7.9 MB] || 13636_Planet_Patrol_ProRes_3840x2160_2997.mov (3840x2160) [3.6 GB] || 13636_Planet_Patrol_4k.mp4 (3840x2160) [114.2 MB] || 13636_Planet_Patrol_SRT_Captions.en_US.srt [878 bytes] || 13636_Planet_Patrol_SRT_Captions.en_US.vtt [890 bytes] || ",
            "hits": 79
        },
        {
            "id": 13663,
            "url": "https://svs.gsfc.nasa.gov/13663/",
            "result_type": "Produced Video",
            "release_date": "2020-08-11T11:00:00-04:00",
            "title": "TESS Completes Its Primary Mission",
            "description": "NASA’s Transiting Exoplanet Survey Satellite (TESS) has completed its two-year primary mission and is continuing its search for new worlds. Watch to review some of TESS’s most interesting discoveries so far.Credit: NASA’s Goddard Space Flight CenterMusic: \"Drive to Succeed\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || TESS_2_Still.jpg (1920x1080) [661.7 KB] || TESS_2_Still_print.jpg (1024x576) [187.0 KB] || 13663_TESS_2nd_Anniversary_Highlights.mp4 (1920x1080) [215.9 MB] || 13663_TESS_2nd_Anniversary_Highlights_Best.mp4 (1920x1080) [611.5 MB] || 13663_TESS_2nd_Anniversary_Highlights_ProRes_1920x1080_2997.mov (1920x1080) [2.7 GB] || 13663_TESS_2nd_Anniversary_Highlights.webm (1920x1080) [23.4 MB] || TESS_2nd_Anniversary_Highlights_SRT_Captions.en_US.srt [4.0 KB] || TESS_2nd_Anniversary_Highlights_SRT_Captions.en_US.vtt [4.0 KB] || ",
            "hits": 178
        },
        {
            "id": 13510,
            "url": "https://svs.gsfc.nasa.gov/13510/",
            "result_type": "Produced Video",
            "release_date": "2020-01-06T19:15:00-05:00",
            "title": "TESS Satellite Discovered Its First World Orbiting Two Stars",
            "description": "NASA’s Transiting Exoplanet Survey Satellite found its first circumbinary planet, a world orbiting two stars 1,300 light-years away. Watch to learn more about this Saturn-size world called TOI 1338 b.Credit: NASA's Goddard Space Flight CenterMusic: \"Albatross\" from Universal Production Music.Complete transcript available.Watch this video on the NASA Goddard YouTube channel. || TOI_1338b_video_still.jpg (1920x1080) [389.2 KB] || TOI_1338b_video_still_print.jpg (1024x576) [128.2 KB] || TOI_1338b_video_still_searchweb.png (320x180) [75.4 KB] || TOI_1338b_video_still_web.png (320x180) [75.4 KB] || TOI_1338b_video_still_thm.png (80x40) [7.0 KB] || TOI_1338b_video_HQ.mp4 (1920x1080) [200.1 MB] || TOI_1338b_video_LQ.mp4 (1920x1080) [107.2 MB] || TOI_1338b_video_prores.mov (1920x1080) [1.0 GB] || TOI_1338b_video_LQ.webm (1920x1080) [12.1 MB] || TOI_1338b_video.en_US.srt [2.0 KB] || TOI_1338b_video.en_US.vtt [2.0 KB] || ",
            "hits": 294
        },
        {
            "id": 13512,
            "url": "https://svs.gsfc.nasa.gov/13512/",
            "result_type": "Produced Video",
            "release_date": "2020-01-06T19:15:00-05:00",
            "title": "TESS Shows Ancient North Star Has Eclipses",
            "description": "This animation illustrates a preliminary model of the Thuban system, now known to be an eclipsing binary thanks to data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The stars orbit every 51.4 days at an average distance slightly greater than Mercury’s distance from the Sun. We view the system about three degrees above the stars’ orbital plane, so they undergo mutual eclipses, but neither is ever completely covered up by its partner. The primary star is 4.3 times bigger than the Sun and has a surface temperature around 17,500 degrees Fahrenheit (9,700 C), making it 70% hotter than our Sun. Its companion, which is five times fainter, is most likely half the primary’s size and 40% hotter than the Sun. Thuban, also called Alpha Draconis, is located about 270 light-years away in the northern constellation Draco.Credit: NASA's Goddard Space Flight Center/Chris Smith (USRA)Watch this video on the NASA.gov Video YouTube channel. || partially_eclipsing_binary_still.jpg (1920x1080) [236.1 KB] || partially_eclipsing_binary_still_print.jpg (1024x576) [95.3 KB] || partially_eclipsing_binary_still_searchweb.png (320x180) [57.6 KB] || partially_eclipsing_binary_still_web.png (320x180) [57.6 KB] || partially_eclipsing_binary_still_thm.png (80x40) [5.1 KB] || partially_eclipsing_binary_HQ.mp4 (1920x1080) [68.5 MB] || partially_eclipsing_binary_LQ.mp4 (1920x1080) [36.6 MB] || partially_eclipsing_binary_prores.mov (1920x1080) [294.3 MB] || partially_eclipsing_binary_LQ.webm (1920x1080) [3.4 MB] || partially_eclipsing_binary_LQ.en_US.vtt [64 bytes] || ",
            "hits": 128
        },
        {
            "id": 13419,
            "url": "https://svs.gsfc.nasa.gov/13419/",
            "result_type": "Animation",
            "release_date": "2019-11-07T13:00:00-05:00",
            "title": "NICER Catches Milestone X-ray Burst",
            "description": "At about 10:04 p.m. EDT on Aug. 20, NASA’s Neutron star Interior Composition Explorer (NICER) telescope on the International Space Station detected a sudden spike of X-rays caused by a massive thermonuclear flash on the surface of a pulsar, the crushed remains of a star that long ago exploded as a supernova. The X-ray burst, the brightest seen by NICER so far, came from an object named SAX J1808.4-3658, or J1808 for short. The observations reveal many phenomena that have never been seen together in a single burst. In addition, the subsiding fireball briefly brightened again for reasons astronomers cannot yet explain.  The data reveal a two-step change in brightness, which scientists think is caused by the ejection of separate layers from the pulsar surface, and other features that will help them decode the physics of these powerful events.The explosion, which astronomers classify as a Type I X-ray burst, released as much energy in 20 seconds as the Sun does in nearly 10 days.J1808 is located about 11,000 light-years away in the constellation Sagittarius, spins at a dizzying 401 rotations each second, and is one member of a binary system. Its companion is a brown dwarf, an object larger than a giant planet yet too small to be a star. A steady stream of hydrogen gas flows from the companion toward the neutron star, and it accumulates in a vast storage structure called an accretion disk.Hydrogen raining onto the pulsar's surface forms a hot, ever-deepening global “sea.” At the base of this layer, temperatures and pressures increase until hydrogen nuclei fuse to form helium nuclei, which produces energy — a process at work in the core of our Sun.     The helium settles out and builds up a layer of its own. Eventually, the conditions allow helium nuclei to fuse into carbon. The helium erupts explosively and unleashes a thermonuclear fireball across the entire pulsar surface.As the burst started, NICER data show that its X-ray brightness leveled off for almost a second before increasing again at a slower pace. The researchers interpret this “stall” as the moment when the energy of the blast built up enough to blow the pulsar’s hydrogen layer into space. The fireball continued to build for another two seconds and then reached its peak, blowing off the more massive helium layer. The helium expanded faster, overtook the hydrogen layer before it could dissipate, and then slowed, stopped and settled back down onto the pulsar’s surface. Following this phase, the pulsar briefly brightened again by roughly 20 percent for reasons the team does not yet understand. || ",
            "hits": 90
        },
        {
            "id": 12989,
            "url": "https://svs.gsfc.nasa.gov/12989/",
            "result_type": "Produced Video",
            "release_date": "2018-07-03T11:00:00-04:00",
            "title": "Superstar Eta Carinae Shoots Cosmic Rays",
            "description": "Zoom into Eta Carinae, where the outflows of two massive stars collide and shoot accelerated particles  cosmic rays  into space.Credit: NASA’s Goddard Space Flight Center  Music: \"Expectant Aspect\" from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || Eta_Car_CR_Still.jpg (1920x1080) [307.1 KB] || Eta_Car_CR_Still_print.jpg (1024x576) [127.9 KB] || Eta_Car_CR_Still_searchweb.png (320x180) [98.2 KB] || Eta_Car_CR_Still_thm.png (80x40) [7.3 KB] || 12989_Eta_Car_CosmicRay_ProRes_1080.webm (1920x1080) [16.1 MB] || 12989_Eta_Car_CosmicRay_1080.m4v (1920x1080) [155.6 MB] || 12989_Eta_Car_CosmicRay_1080.mp4 (1920x1080) [234.6 MB] || 12989_Eta_Car_CosmicRay_1080p.mov (1920x1080) [311.6 MB] || 12989_Eta_Car_CosmicRay_SRT_Captions.en_US.srt [2.0 KB] || 12989_Eta_Car_CosmicRay_SRT_Captions.en_US.vtt [2.0 KB] || 12989_Eta_Car_CosmicRay_ProRes_1080.mov (1920x1080) [2.1 GB] || ",
            "hits": 208
        },
        {
            "id": 12399,
            "url": "https://svs.gsfc.nasa.gov/12399/",
            "result_type": "Produced Video",
            "release_date": "2016-10-27T12:55:00-04:00",
            "title": "NASA's Kepler, Swift Missions Harvest ‘Pumpkin’ Stars",
            "description": "Dive into the Kepler field and learn more about the origins of these rapidly spinning stars.Credit: NASA's Goddard Space Flight CenterMusic: \"Electric Cosmos\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Pumpkin_Star_Still.png (1920x1080) [10.8 MB] || Pumpkin_Star_Still_print.jpg (1024x576) [85.7 KB] || Pumpkin_Star_Still_searchweb.png (320x180) [66.5 KB] || Pumpkin_Star_Still_thm.png (80x40) [4.4 KB] || 12399_Swift_Pumpkin_Star2_ProRes_1920x1080_2997.mov (1920x1080) [2.0 GB] || 12399_Swift_Pumpkin_Star_FINAL2_youtube_hq.mov (1920x1080) [1.2 GB] || 12399_Swift_Pumpkin_Star2_H264_1080.mov (1920x1080) [221.8 MB] || 12399_Swift_Pumpkin_Star2_1080_Good.m4v (1920x1080) [147.1 MB] || 12399_Swift_Pumpkin_Star2_1080_Most_Compatible.m4v (960x540) [59.7 MB] || 12399_Swift_Pumpkin_Star_FINAL2_HD.wmv (1920x1080) [332.6 MB] || 12399_Swift_Pumpkin_Star2_ProRes_1920x1080_2997.webm (1920x1080) [17.0 MB] || 12399_Swift_Pumpkin_Star_SRT_Captions.en_US.srt [2.3 KB] || 12399_Swift_Pumpkin_Star_SRT_Captions.en_US.vtt [2.3 KB] || 12399_Swift_Pumpkin_Star_FINAL2_ipod_sm.mp4 (320x240) [26.8 MB] || ",
            "hits": 133
        },
        {
            "id": 11895,
            "url": "https://svs.gsfc.nasa.gov/11895/",
            "result_type": "Produced Video",
            "release_date": "2015-07-02T10:00:00-04:00",
            "title": "Astronomers Predict Cosmic Light Show from 2018 Stellar Encounter",
            "description": "Coming attraction: Astronomers are expecting high-energy explosions when pulsar J2032 swings around its massive companion star in early 2018. The pulsar will plunge through a disk of gas and dust surrounding the star, triggering cosmic fireworks. Scientists are planning a global campaign to watch the event across the spectrum, from radio waves to gamma rays. Credit: NASA's Goddard Space Flight CenterWatch this video on the NASA Goddard YouTube channel.For complete transcript, click here. || Binary_Pulsar_Still.png (1920x1080) [2.0 MB] || Binary_Pulsar_Still_print.jpg (1024x576) [88.4 KB] || Binary_Pulsar_Still_searchweb.png (320x180) [74.7 KB] || Binary_Pulsar_Still_thm.png (80x40) [8.1 KB] || 11895_Fermi_Binary_Pulsar_.mov (1920x1080) [1.5 GB] || 11895_Fermi_Binary_Pulsar_-H264_Best_1920x1080_29.97.mov (1920x1080) [523.1 MB] || 11895_Fermi_Binary_Pulsar_-H264_Good_1080_29.97.mov (1920x1080) [77.1 MB] || YOUTUBE_HQ_G2015-051_Fermi_Binary_Pulsar_FINAL_VX-171746_youtube_hq.mov (1280x720) [174.9 MB] || 11895_Fermi_Binary_Pulsar_MPEG4_1920X1080_2997.mp4 (1920x1080) [53.1 MB] || WMV_G2015-051_Fermi_Binary_Pulsar_FINAL_VX-171746_1280x720.wmv (1280x720) [48.3 MB] || APPLE_TV_G2015-051_Fermi_Binary_Pulsar_FINAL_VX-171746_appletv.m4v (1280x720) [71.5 MB] || 11895_Fermi_Binary_Pulsar_.webm (1920x1080) [14.4 MB] || APPLE_TV_G2015-051_Fermi_Binary_Pulsar_FINAL_VX-171746_appletv_subtitles.m4v (1280x720) [71.6 MB] || 11895_Fermi_Binary_Pulsar_SRT_Captions.en_US.srt [1.8 KB] || 11895_Fermi_Binary_Pulsar_SRT_Captions.en_US.vtt [1.8 KB] || ",
            "hits": 74
        },
        {
            "id": 20225,
            "url": "https://svs.gsfc.nasa.gov/20225/",
            "result_type": "Animation",
            "release_date": "2015-07-02T10:00:00-04:00",
            "title": "Binary Pulsar J2032 animation",
            "description": "Binary Pulsar J2032 animation || BinaryPulsar.png (1920x1080) [2.0 MB] || Cam1_00312_print.jpg (1024x576) [65.8 KB] || Cam1_00312_searchweb.png (320x180) [68.9 KB] || Cam1_00312_thm.png (80x40) [5.7 KB] || BinaryPulsar_1080p60.webm (1920x1080) [2.1 MB] || 1920x1080_16x9_60p (1920x1080) [32.0 KB] || BinaryPulsar_1080p60.mp4 (1920x1080) [11.6 MB] || Bin_pulsar_442.mov (1920x1080) [534.0 MB] || Bin_pulsar_H264.mov (1920x1080) [315.4 MB] || ",
            "hits": 218
        },
        {
            "id": 11804,
            "url": "https://svs.gsfc.nasa.gov/11804/",
            "result_type": "Produced Video",
            "release_date": "2015-05-14T14:00:00-04:00",
            "title": "RXTE Data Link Pulsar Pulses with a QPO",
            "description": "This animation illustrates the direct relationship between a pulsar's X-ray pulses and its quasi-periodic oscillation (QPO), a flickering signal that hovers around certain frequencies. The QPO is shown here as a bright patch near the inner edge of the disk of gas that feeds matter to the pulsar at the center, called SAX J1808. Guided by magnetic fields, gas streaming onto the neutron star forms bright hot spots. As the pulsar spins 401 times a second, telescopes detect X-ray pulses as these locations swing into view from Earth. When the QPO orbits more slowly than the pulsar’s spin, the neutron star’s magnetic field holds back flowing gas, dimming the X-ray pulses. But during an outburst, the inner edge of the disk is forced closer to the pulsar, resulting in a faster-moving QPO and compression of the pulsar's magnetic field. When the QPO matches or bests the pulsar’s spin, more gas streams onto the neutron star, and the pulses brighten. Gas may even flow directly onto the pulsar's equatorial region, producing extra hot spots. NASA’s Rossi X-ray Timing Explorer observed this relationship during outbursts in 2002, 2005, and 2008. Credit: NASA's Goddard Space Flight Center Conceptual Image Lab || QPO_16bit_00728_print.jpg (1024x576) [96.1 KB] || QPO_16bit_00728_web.jpg (320x180) [16.6 KB] || QPO_16bit_00728_thm.png (80x40) [7.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || 11804_RXTE_QPO_H264_Good_1920x1080_2997.mov (1920x1080) [45.4 MB] || 11804_RXTE_QPO_MPEG4_1920X1080_2997.mp4 (1920x1080) [28.0 MB] || QPO_16bit_00728.tif (1920x1080) [11.9 MB] || 11804_RXTE_QPO_H264_Good_1920x1080_2997.webm (1920x1080) [3.9 MB] || 11804_RXTE_QPO_H264_Best_1920x1080_2997.mov (1920x1080) [240.9 MB] || 11804_RXTE_QPO_ProRes_1920x1080_2997.mov (1920x1080) [416.6 MB] || ",
            "hits": 60
        },
        {
            "id": 11725,
            "url": "https://svs.gsfc.nasa.gov/11725/",
            "result_type": "Produced Video",
            "release_date": "2015-01-07T13:15:00-05:00",
            "title": "NASA Missions Take an Unparalleled Look into Superstar Eta Carinae",
            "description": "Explore Eta Carinae from the inside out with the help of supercomputer simulations and data from NASA satellites and ground-based observatories. Credit: NASA's Goddard Space Flight CenterWatch this video on the NASA Goddard YouTube channel.For complete transcript, click here. || Eta_Car_Density_XY_R10_R100_STILL_1920.jpg (1920x1080) [804.4 KB] || Eta_Car_Density_XY_R10_R100_STILL_1920_print.jpg (1024x576) [52.0 KB] || Eta_Car_Density_XY_R10_R100_STILL.jpg (4928x2772) [874.1 KB] || Eta_Car_Density_XY_R10_R100_STILL.png (4928x2772) [36.6 MB] || Eta_Car_Density_XY_R10_R100_STILL_1920_web.jpg (320x180) [13.1 KB] || Eta_Car_Density_XY_R10_R100_STILL_1920_searchweb.png (320x180) [55.9 KB] || Eta_Car_Density_XY_R10_R100_STILL_1920_thm.png (80x40) [8.0 KB] || Eta_Car_Density_XY_R10_R100_STILL_1920.tiff (1920x1080) [11.9 MB] || G2015-001_Eta_Car_Binary_Final_appletv.webm (960x540) [30.5 MB] || G2015-001_Eta_Car_Binary_Final_ipod_lg.m4v (640x360) [43.2 MB] || G2015-001_Eta_Car_Binary.en_US.vtt [5.2 KB] || G2015-001_Eta_Car_Binary.en_US.srt [5.2 KB] || G2015-001_Eta_Car_Binary_Final_ipod_sm.mp4 (320x240) [22.8 MB] || G2015-001_Eta_Car_Binary_Final_appletv_subtitles.m4v (960x540) [103.9 MB] || G2015-001_Eta_Car_Binary_Final_appletv.m4v (960x540) [104.0 MB] || G2015-001_Eta_Car_Binary_Final_1280x720.wmv (1280x720) [107.6 MB] || 11725_Eta_Car_Binary2_MPEG4_1920X1080_2997.mp4 (1920x1080) [116.9 MB] || 11725_Eta_Car_Binary2_ProRes_1920x1080_2997.mov (1920x1080) [3.5 GB] || 11725_Eta_Car_Binary2_H264_Best_1920x1080_2997.mov (1920x1080) [2.6 GB] || 11725_Eta_Car_Binary2_H264_Good_1920x1080_2997.mov (1920x1080) [506.2 MB] || Eta_Car_Density_XY_R10_R100_STILL.tiff (4928x2772) [104.2 MB] || ",
            "hits": 138
        },
        {
            "id": 11722,
            "url": "https://svs.gsfc.nasa.gov/11722/",
            "result_type": "Produced Video",
            "release_date": "2015-01-07T13:00:00-05:00",
            "title": "Supercomputer Simulations of Eta Carinae",
            "description": "Density simulation. This movie shows a wide view of the system looking down on the orbital plane of the two stars, which are located at the center. The view spans 3,200  times the average distance between Earth and the sun, or 298 billion miles (478 billion kilometers). Lighter colors indicate greater densities, with the highest densities occurring near the primary and in the wind interaction region. The faster wind of the smaller star carves a spiral cavity into the dense wind of the primary star, and this structure expands outward with the primary wind at about 1 million mph (1.6 million km/h. || R100_density_xy_axes_and_colorbar_print.jpg (1024x1024) [84.9 KB] || R100_density_xy_axes_and_colorbar.png (4096x4096) [2.8 MB] || R100_density_xy_axes_and_colorbar_web.jpg (320x320) [17.8 KB] || Eta_Car_R100_Density_XY_H264_Good_1024x1024_searchweb.png (320x180) [57.8 KB] || Eta_Car_R100_Density_XY_H264_Good_1024x1024.mov (1024x1024) [3.8 MB] || Eta_Car_R100_Density_XY_H264_Good_1024x1024.webm (1024x1024) [2.4 MB] || Eta_Car_R100_Density_XY_4k.mov (4096x4096) [876.4 MB] || ",
            "hits": 80
        },
        {
            "id": 11531,
            "url": "https://svs.gsfc.nasa.gov/11531/",
            "result_type": "Produced Video",
            "release_date": "2014-09-30T14:00:00-04:00",
            "title": "Swift Catches Mega Flares from a Mini Star",
            "description": "On April 23, NASA's Swift satellite detected the strongest, hottest, and longest-lasting sequence of stellar flares ever seen from a nearby red dwarf star. The initial blast from this record-setting series of explosions was as much as 10,000 times more powerful than the largest solar flare ever recorded. At its peak, the flare reached temperatures of 360 million degrees Fahrenheit (200 million Celsius), more than 12 times hotter than the center of the sun. The \"superflare\" came from one of the stars in a close binary system known as DG Canum Venaticorum, or DG CVn for short, located about 60 light-years away. Both stars are dim red dwarfs with masses and sizes about one-third of our sun's. They orbit each other at about three times Earth's average distance from the sun, which is too close for Swift to determine which star erupted. At 5:07 p.m. EDT on April 23, the rising tide of X-rays from DG CVn's superflare triggered Swift's Burst Alert Telescope (BAT). Swift turned to observe the source in greater detail with other instruments and, at the same time, notified astronomers around the globe that a powerful outburst was in progress.For about three minutes after the BAT trigger, the superflare's X-ray brightness was greater than the combined luminosity of both stars at all wavelengths under normal conditions.The largest solar explosions are classified as extraordinary, or X class, solar flares based on their X-ray emission. The biggest flare ever seen from the sun occurred in November 2003 and is rated as X 45. But if the flare on DG CVn were viewed from a planet the same distance as Earth is from the sun and measured the same way, it would have been ranked 10,000 times greater, at about X 100,000. How can a star just a third the size of the sun produce such a giant eruption? The key factor is its rapid spin, a crucial ingredient for amplifying magnetic fields. The flaring star in DG CVn rotates in under a day, about 30 or more times faster than our sun. The sun also rotated much faster in its youth and may well have produced superflares of its own, but, fortunately for us, it no longer appears capable of doing so. || ",
            "hits": 125
        },
        {
            "id": 11608,
            "url": "https://svs.gsfc.nasa.gov/11608/",
            "result_type": "Produced Video",
            "release_date": "2014-07-31T14:00:00-04:00",
            "title": "Fermi Reveals Novae as a New Class of Gamma-Ray Sources",
            "description": "Observations of four stellar eruptions, called novae, by NASA's Fermi Gamma-ray Space Telescope firmly establish that these relatively common outbursts nearly always produce gamma rays, the most energetic form of light. A nova is a sudden, short-lived brightening of an otherwise inconspicuous star caused by a thermonuclear explosion on the surface of a white dwarf, a compact star not much larger than Earth. Novae occur because a stream of gas flowing from the star continually piles up into a layer on the white dwarf's surface. This layer eventually reaches a flash point and detonates in a runaway thermonuclear explosion. Each nova releases up to 100,000 times the annual energy output of our sun. Prior to Fermi, no one suspected these outbursts were capable of producing high-energy gamma rays. Such emission, with energies millions of times greater than visible light, usually is associated with far more powerful cosmic blasts.Fermi's Large Area Telescope (LAT) scored its first nova detection in March 2010 with an outburst of V407 Cygni. In this rare type of system, a white dwarf interacts with a red giant star more than a hundred times the size of our sun. Other members of this unusual stellar class have been observed to \"go nova\" every few decades.In 2012 and 2013, the LAT found three much more typical, or \"classical,\" novae: V339 Delphini in 2013 and V1324 Scorpii and V959 Monocerotis in 2012. The outbursts occurred in comparatively common systems where a white dwarf and a sun-like star orbit each other every few hours. Astronomers estimate that between 20 and 50 novae occur each year in our galaxy. Most go undetected, their visible light obscured by intervening dust and their gamma rays dimmed by distance. All of the gamma-ray novae found so far lie between 9,000 and 15,000 light-years away, which is relatively nearby compared to our galaxy's size.One explanation for the gamma-ray emission is that the blast creates multiple shock waves, which expand into space at slightly different speeds. Faster shocks could interact with slower ones, accelerating particles to near the speed of light. These particles ultimately could produce gamma rays. || ",
            "hits": 131
        },
        {
            "id": 11567,
            "url": "https://svs.gsfc.nasa.gov/11567/",
            "result_type": "Produced Video",
            "release_date": "2014-07-22T10:00:00-04:00",
            "title": "PSR J1023, A 'Transformer' Pulsar—Animations",
            "description": "Pulsar J1023 is a member of an exceptional binary system containing a rapidly spinning neutron star. In June 2013, the pulsar underwent a dramatic change in behavior never before observed. Its radio beacon vanished, while at the same time the system brightened significantly in gamma rays, the highest-energy form of light.The stellar system, known as AY Sextantis and located about 4,400 light-years away in the constellation Sextans, pairs a 1.7-millisecond pulsar named PSR J1023+0038 — J1023 for short — with a star containing about one-fifth the mass of the sun. The stars complete an orbit in only 4.8 hours, which places them so close together that a high-energy \"wind\" of charged particles from the pulsar is gradually evaporating its companion. What's happening, astronomers say, are the last sputtering throes of the pulsar spin-up process, where a flow of matter from the companion has, over millions of years, dramatically increased the pulsar's rotation. J1023 now spins at about 35,000 rpm, but the gas stream from the companion is no longer continuous. Researchers regard the system as a unique laboratory for understanding how millisecond pulsars form and for studying details of how accretion takes place on neutron stars. || ",
            "hits": 344
        },
        {
            "id": 11609,
            "url": "https://svs.gsfc.nasa.gov/11609/",
            "result_type": "Produced Video",
            "release_date": "2014-07-22T10:00:00-04:00",
            "title": "NASA's Fermi Catches a 'Transformer' Pulsar",
            "description": "In late June 2013, an exceptional binary system containing a rapidly spinning neutron star underwent a dramatic change in behavior never before observed. The pulsar's radio beacon vanished, while at the same time the system brightened fivefold in gamma rays, the most powerful form of light, according to measurements by NASA's Fermi Gamma-ray Space Telescope.The system, known as AY Sextantis, is located about 4,400 light-years away in the constellation Sextans. It pairs a 1.7-millisecond pulsar named PSR J1023+0038 — J1023 for short — with a star containing about one-fifth the mass of the sun. The stars complete an orbit in only 4.8 hours, which places them so close together that the pulsar will gradually evaporate its companion. To better understand J1023's spin and orbital evolution, the system was routinely monitored in radio. These observations revealed that the pulsar's radio signal had turned off and prompted the search for an associated change in its gamma-ray properties.What's happening, astronomers say, are the last sputtering throes of the pulsar spin-up process. Researchers regard the system as a unique laboratory for understanding how millisecond pulsars form and for studying details of how accretion takes place on neutron stars. In J1023, the stars are close enough that a stream of gas flows from the sun-like star toward the pulsar. The pulsar's rapid rotation and intense magnetic field are responsible for both the radio beam and its powerful pulsar wind. When the radio beam is detectable, the pulsar wind holds back the companion's gas stream, preventing it from approaching too closely. But now and then the stream surges, pushing its way closer to the pulsar and establishing an accretion disk. When gas from the disk falls to an altitude of about 50 miles (80 km), processes involved in creating the radio beam are either shut down or, more likely, obscured. Some of the gas may be accelerated outward at nearly the speed of light, forming dual particle jets firing in opposite directions. Shock waves within and along the periphery of these jets are a likely source of the bright gamma-ray emission detected by Fermi. || ",
            "hits": 108
        },
        {
            "id": 11215,
            "url": "https://svs.gsfc.nasa.gov/11215/",
            "result_type": "Produced Video",
            "release_date": "2014-02-20T11:00:00-05:00",
            "title": "PSR J1311-3430 'Black Widow' Pulsar Animations",
            "description": "The essential features of black widow binaries, and their cousins, known as redbacks, are that they place a normal but very low-mass star in close proximity to a millisecond pulsar, which has disastrous consequences for the star. Black widow systems contain stars that are both physically smaller and of much lower mass than those found in redbacks.So far, astronomers have found at least 18 black widows and nine redbacks within the Milky Way, and additional members of each class have been discovered within the dense globular star clusters that orbit our galaxy. These animations show artist's impressions of one system, named PSR J1311-3430. Discovered in 2012, J1311 sets the record for the tightest orbit of its class and contains one of the heaviest neutron stars known. The pulsar's featherweight companion, which is only a dozen or so times the mass of Jupiter and just 60 percent of its size, completes an orbit every 93 minutes – less time than it takes to watch most movies. Recent studies allow a range of values extending down to 2 solar masses for the pulsar, still among the highest-known for neutron stars. || ",
            "hits": 256
        },
        {
            "id": 11216,
            "url": "https://svs.gsfc.nasa.gov/11216/",
            "result_type": "Produced Video",
            "release_date": "2014-02-20T11:00:00-05:00",
            "title": "Black Widow Pulsars Consume Their Mates",
            "description": "Black widow spiders and their Australian cousins, known as redbacks, are notorious for an unsettling tendency to kill and devour their male partners. Astronomers have noted similar behavior among two rare breeds of binary system that contain rapidly spinning neutron stars, also known as pulsars. The essential features of black widow and redback binaries are that they place a normal but very low-mass star in close proximity to a millisecond pulsar, which has disastrous consequences for the star. Black widow systems contain stars that are both physically smaller and of much lower mass than those found in redbacks.So far, astronomers have found at least 18 black widows and nine redbacks within the Milky Way, and additional members of each class have been discovered within the dense globular star clusters that orbit our galaxy. One black widow system, named PSR J1311-3430 and discovered in 2012, sets the record for the tightest orbit of its class and contains one of the heaviest neutron stars known. The pulsar's featherweight companion, which is only a dozen or so times the mass of Jupiter and just 60 percent of its size, completes an orbit every 93 minutes – less time than it takes to watch most movies. The side of the star facing the pulsar is heated to more than 21,000 degrees Fahrenheit (nearly 12,000 C), or more than twice as hot as the sun's surface. Recent studies allow a range of values extending down to 2 solar masses for the pulsar, making it one of the most massive neutron stars known. Watch the video to learn more about this system and its discovery from some of the scientists involved. || ",
            "hits": 65
        },
        {
            "id": 11109,
            "url": "https://svs.gsfc.nasa.gov/11109/",
            "result_type": "Produced Video",
            "release_date": "2012-10-12T10:00:00-04:00",
            "title": "X-ray Satellites Monitor the Clashing Winds of a Colossal Binary",
            "description": "One of the nearest and richest OB associations in our galaxy is Cygnus OB2, which is located about 4,700 light-years away and hosts some 3,000 hot stars, including about 100 in the O class. Weighing in at more than a dozen times the sun's mass and sporting surface temperatures five to ten times hotter, these ginormous blue-white stars blast their surroundings with intense ultraviolet light and powerful outflows called stellar winds. Two of these stars can be found in the intriguing binary system known as Cygnus OB2 #9. In 2011, NASA's Swift satellite, the European Space Agency's XMM-Newton observatory and several ground-based facilities took part in a campaign to monitor the system as the giant stars raced toward their closest approach. The observations are giving astronomers a more detailed picture of the stars, their orbits and the interaction of their stellar winds. An O-type star is so luminous that the pressure of its starlight actually drives material from its surface, creating particle outflows with speeds of several million miles an hour. Put two of these humongous stars in the same system and their winds can collide during all or part of the orbit, creating both radio emission and X-rays.In 2008, research showed that Cygnus OB2 #9 emitted radio signals that varied every 2.355 years. In parallel, Yael Naz || ",
            "hits": 91
        },
        {
            "id": 11110,
            "url": "https://svs.gsfc.nasa.gov/11110/",
            "result_type": "Produced Video",
            "release_date": "2012-10-05T14:00:00-04:00",
            "title": "X-ray Nova Flaring Black Hole animation",
            "description": "An X-ray nova is a short-lived X-ray source that appears suddenly, reaches its emission peak in a few days and then fades out over a period of months. The outburst arises when a torrent of stored gas suddenly rushes toward one of the most compact objects known, either a neutron star or a black hole. || ",
            "hits": 91
        },
        {
            "id": 10869,
            "url": "https://svs.gsfc.nasa.gov/10869/",
            "result_type": "Produced Video",
            "release_date": "2012-01-10T11:00:00-05:00",
            "title": "NASA's RXTE Helps Pinpoint Launch of 'Bullets' in a Black Hole's Jet",
            "description": "Using observations from NASA's Rossi X-ray Timing Explorer (RXTE) satellite and the National Science Foundation's (NSF) Very Long Baseline Array (VLBA) radio telescope, an international team of astronomers has identified the moment when a black hole in our galaxy launched superfast knots of gas into space. Racing outward at about one-quarter the speed of light, these \"bullets\" of ionized gas are thought to arise from a region located just outside the black hole's event horizon, the point beyond which nothing can escape.The research centered on the mid-2009 outburst of a binary system known as H1743-322, located about 28,000 light-years away toward the constellation Scorpius. Discovered by NASA's HEAO-1 satellite in 1977, the system is composed of a normal star and a black hole of modest but unknown masses. Their orbit around each other is measured in days, which puts them so close together that the black hole pulls a continuous stream of matter from its stellar companion. The flowing gas forms a flattened accretion disk millions of miles across, several times wider than our sun, centered on the black hole. As matter swirls inward, it is compressed and heated to tens of millions of degrees, so hot that it emits X-rays.Some of the infalling matter becomes re-directed out of the accretion disk as dual, oppositely directed jets. Most of the time, the jets consist of a steady flow of particles. Occasionally, though, they morph into more powerful outflows that hurl massive gas blobs at significant fractions of the speed of light. || ",
            "hits": 60
        },
        {
            "id": 10875,
            "url": "https://svs.gsfc.nasa.gov/10875/",
            "result_type": "Produced Video",
            "release_date": "2011-12-15T10:00:00-05:00",
            "title": "RXTE Detects 'Heartbeat' Of Smallest Black Hole Candidate",
            "description": "Data from NASA's Rossi X-ray Timing Explorer (RXTE) satellite has identified a candidate for the smallest-known black hole. The evidence comes from a specific type of X-ray pattern — nicknamed a \"heartbeat\" because of its resemblance to an electrocardiogram — that until now has been recorded in only one other black hole system. Named IGR J17091-3624 after the astronomical coordinates of its sky position, the binary system pairs a normal star with a black hole that may weigh less than three times the sun's mass, near the theoretical boundary where black-hole status first becomes possible. Flare-ups occur when gas from the normal star streams toward the black hole and forms a disk around it. Friction within the disk heats the gas to millions of degrees, which is hot enough to radiate X-rays.The record-holder for ubiquitous X-ray variability is another black hole binary named GRS 1915+105. This system is unique in displaying more than a dozen highly structured patterns — typically lasting between seconds and hours — that scientists distinguish by Greek-letter names. Seven of these patterns are now seen in IGR J17091, including the so-called rho-class oscillations that astronomers describe them as the \"heartbeat\" of black hole systems.It's thought that strong magnetic fields near the black hole's event horizon eject some of the gas into dual, oppositely directed jets that blast outward at nearly the speed of light. The peak of its heartbeat emission corresponds to the emergence of the jet. Changes in the X-ray spectrum observed by RXTE during each beat in GRS 1915 reveal that the innermost region of the disk emits enough radiation to push back the gas, creating a strong outward wind that staunches the inward flow, briefly starving the black hole and shutting down the jet. This corresponds to the faintest emission. Eventually the inner disk gets so bright and so hot that it essentially disintegrates and plunges toward the black hole, re-establishing the jet and beginning the cycle anew. In GRS 1915+105, which at 14 solar masses is by for the more massive of the two, this cycle can take as little as 40 seconds. In IGR J17091, the emission can be 20 times fainter than GRS 1915, and the heartbeat cycle can occur up to eight times faster.Download the animations here. || ",
            "hits": 52
        },
        {
            "id": 10876,
            "url": "https://svs.gsfc.nasa.gov/10876/",
            "result_type": "Produced Video",
            "release_date": "2011-12-15T10:00:00-05:00",
            "title": "Black Hole Pulse Animation",
            "description": "Animations associated with the RXTE Black Hole 'Heartbeat' release.View the short video using these animations here. || ",
            "hits": 131
        },
        {
            "id": 10798,
            "url": "https://svs.gsfc.nasa.gov/10798/",
            "result_type": "Produced Video",
            "release_date": "2011-06-29T10:00:00-04:00",
            "title": "Stellar Odd Couple Makes Striking Flares",
            "description": "Every 3.4 years, pulsar B1259-63 dives twice through the gas disk surrounding the massive blue star it orbits. With each pass, it produces gamma rays. During the most recent event, NASA's Fermi Gamma-ray Space Telescope observed that the pulsar's gamma-ray flare was much more intense the second time it plunged through the disk. Astronomers don't yet know why.For the B1259 binary animation, go here. || ",
            "hits": 40
        },
        {
            "id": 10802,
            "url": "https://svs.gsfc.nasa.gov/10802/",
            "result_type": "Produced Video",
            "release_date": "2011-06-28T10:00:00-04:00",
            "title": "B1259-63 Binary Animation",
            "description": "Animation of the B1259-63 binary system with a pulsar that emits gamma rays as it passes through the gas disk around a blue giant.For a short narrated video and stills about this system, go here. || ",
            "hits": 49
        },
        {
            "id": 10625,
            "url": "https://svs.gsfc.nasa.gov/10625/",
            "result_type": "Produced Video",
            "release_date": "2010-08-17T08:00:00-04:00",
            "title": "RXTE Sees Eclipses from Fast X-ray Pulsar",
            "description": "Astronomers using NASA's Rossi X-ray Timing Explorer (RXTE) have found the first fast X-ray pulsar to be eclipsed by its companion star. Further studies of this unique stellar system will shed light on some of the most compressed matter in the universe and test a key prediction of Einstein's relativity theory.Known as Swift J1749.4-2807 — J1749 for short — the system erupted with an X-ray outburst on April 10. During the event, RXTE observed three eclipses, detected X-ray pulses that identified the neutron star as a pulsar, and even recorded pulse variations that indicated the neutron star's orbital motion. More information here. || ",
            "hits": 76
        },
        {
            "id": 20184,
            "url": "https://svs.gsfc.nasa.gov/20184/",
            "result_type": "Animation",
            "release_date": "2010-08-12T00:00:00-04:00",
            "title": "Fermi Sees a Nova",
            "description": "NASA's Fermi Gamma-ray Space Telescope has detected gamma-rays from a nova for the first time. The finding stunned observers and theorists alike because it overturns a long-standing notion that novae explosions lack the power for such high-energy emissions. In March, Fermi's Large Area Telescope (LAT) detected gamma rays — the most energetic form of light - from the nova for 15 days. Scientists believe that the emission arose as a million-mile-per-hour shock wave raced from the site of the explosion. A nova is a sudden, short-lived brightening of an otherwise inconspicuous star. The outburst occurs when a white dwarf in a binary system erupts in an enormous thermonuclear explosion. \"In human terms, this was an immensely powerful eruption, equivalent to about 1,000 times the energy emitted by the sun every year,\" said Elizabeth Hays, a Fermi deputy project scientist at NASA's Goddard Space Flight Center in Greenbelt, Md. \"But compared to other cosmic events Fermi sees, it was quite modest. We're amazed that Fermi detected it so strongly.\" More information here. || ",
            "hits": 90
        },
        {
            "id": 10546,
            "url": "https://svs.gsfc.nasa.gov/10546/",
            "result_type": "Produced Video",
            "release_date": "2010-01-26T00:00:00-05:00",
            "title": "Neutron Star and Red Giant Binary Destruction",
            "description": "After a supernova, a binary star may be composed of one red giant and one neutron star. The red giant can be torn apart by the neturon star's gravity if it is too close. || ",
            "hits": 154
        },
        {
            "id": 10531,
            "url": "https://svs.gsfc.nasa.gov/10531/",
            "result_type": "Produced Video",
            "release_date": "2009-11-26T12:59:00-05:00",
            "title": "Fermi telescope detects gamma-rays from Cygnus X-3",
            "description": "In Cygnus X-3, a hot, massive star is paired with a compact object — either a neutron star or a black hole — that blasts twin radio-emitting jets of matter into space at more than half the speed of light. Astronomers call these systems microquasars. Their properties — strong emission across a broad range of wavelengths, rapid brightness changes, and radio jets — resemble miniature versions of distant galaxies (called quasars and blazars) whose emissions are thought to be powered by enormous black holes. Cygnus X-3, first detected in 1966 as among the sky's strongest X-ray sources, was also one of the earliest claimed gamma-ray sources. Efforts to confirm those observations helped spur the development of improved gamma-ray detectors, a legacy culminating in the Large Area Telescope (LAT) aboard NASA's Fermi Gamma-ray Space Telescope. || ",
            "hits": 70
        },
        {
            "id": 10532,
            "url": "https://svs.gsfc.nasa.gov/10532/",
            "result_type": "Produced Video",
            "release_date": "2009-11-23T00:00:00-05:00",
            "title": "Type Ia supernova",
            "description": "A binary star system in which a white dwarf accretes matter from a normal companion star can be a ticking bomb. In this animation, we see such a system from a distance. The white dwarf packs more mass than our sun's into a volume about the size of Earth. Matter streaming from the red star accumulates on the white dwarf until the dwarf explodes. With its partner destroyed, the normal star careens into space. This scenario results in what astronomers refer to as a Type Ia supernova. Because they explode with similar brightness and can be seen across the universe, Type Ia supernovae provide astronomers with information about the distant cosmos. || ",
            "hits": 181
        },
        {
            "id": 10507,
            "url": "https://svs.gsfc.nasa.gov/10507/",
            "result_type": "Produced Video",
            "release_date": "2009-10-28T01:45:00-04:00",
            "title": "Gamma-Rays from High-Mass X-Ray Binaries",
            "description": "In its first year, NASA's Fermi Gamma-ray Space Telescope discovered GeV (billions of electron volts) intensity variations revealing orbital motion in high-mass X-ray binaries (HMXBs). These are systems where a compact companion, such as a neutron star or a black hole, rapidly orbits a hot, young, massive star. The first examples include LSI +61 303, which sports a 26-day orbital period, and LS 5039 (3.9 days). This animation shows such a system. When the compact object lies far from its host star, TeV (trillions of electron volts) gamma-rays (white) are seen by ground-based gamma-ray observatories. But, as the object plunges closer to the star, the TeV emission is quenched and GeV emission turns on. Interactions by accelerated particles from the compact source with gas encircling the star — or in some systems, the star's light itself — is thought to be responsible for this change. || ",
            "hits": 51
        }
    ]
}