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        {
            "id": 5577,
            "url": "https://svs.gsfc.nasa.gov/5577/",
            "result_type": "Animation",
            "release_date": "2025-11-20T09:00:00-05:00",
            "title": "SDO Sun This Week",
            "description": "This visualization shows SDO AIA-304 imagery from the past 7 days with a color table and image processing applied. Archive folders are provided in the Download menu.",
            "hits": 0
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        {
            "id": 14898,
            "url": "https://svs.gsfc.nasa.gov/14898/",
            "result_type": "Produced Video",
            "release_date": "2025-09-15T15:00:00-04:00",
            "title": "Our Home In Space Series",
            "description": "The heliosphere, the massive bubble created by our Sun, is like our “house” in space. It shelters us from harsh weather outside and regulates the environment inside. Without our heliosphere, Earth may never have developed life at all.  But there’s a lot we still don’t know about our cosmic home. How big is it, and what is it shaped like? How does it compare to the “houses” created by other stars? A new NASA mission will soon unlock answers to these questions and more.  Launching as early as Sept. 23, NASA’s Interstellar Mapping and Acceleration Probe will help us construct the “blueprints” or our home in space. This three-part series explores how we learn about our heliosphere, how it protects us, and how it advances the search for life elsewhere in the Universe. || ",
            "hits": 201
        },
        {
            "id": 20409,
            "url": "https://svs.gsfc.nasa.gov/20409/",
            "result_type": "Animation",
            "release_date": "2025-08-22T09:00:00-04:00",
            "title": "The Heliosphere and Galactic Cosmic Rays",
            "description": "Surrounding our solar system is a giant protective bubble created by particles and magnetic fields from the Sun called the heliosphere. Every 11 years, the Sun’s activity ramps up and down in what’s known as the solar cycle. As the Sun reaches its peak activity level, called solar maximum, the heliosphere expands. During this time, the heliosphere’s protective shield is strengthened by the increase in particles and magnetic fields from the Sun. As a result, fewer damaging particles from the galaxy, such as galactic cosmic rays, are able to penetrate into the heliosphere. As the Sun ramps down into a low level of activity, called solar minimum, the heliosphere shrinks and more cosmic rays are able to enter the heliosphere. || ",
            "hits": 437
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        {
            "id": 5344,
            "url": "https://svs.gsfc.nasa.gov/5344/",
            "result_type": "Visualization",
            "release_date": "2024-10-15T14:00:00-04:00",
            "title": "Solar Cycle 25 - the Solar Magnetic Field from Solar Minimum to Pole Flip",
            "description": "One advantage of long-lived missions like Solar Dynamics Observatory (SDO) is the ability to see slow but significant changes over long periods of time.This view from SDO's Helioseismic and Magnetic Imager (HMI) shows the evolution of sunspots on the solar disk starting from solar minimum (around December 2019) and into the maximum solar activity phase.  The video ends in September 2024, however this maximum phase is expected to continue into 2025.",
            "hits": 522
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        {
            "id": 14683,
            "url": "https://svs.gsfc.nasa.gov/14683/",
            "result_type": "Produced Video",
            "release_date": "2024-10-15T13:30:00-04:00",
            "title": "NASA, NOAA Announce That the Sun Has Reached the Solar Maximum Period",
            "description": "In a teleconference with reporters on Tuesday, October 15, 2024, representatives from NASA, the National Oceanic and Atmospheric Agency (NOAA), and the Solar Cycle Prediction Panel announced the Sun has reached its solar maximum period.The solar cycle is the natural cycle of the Sun as it transitions between low and high activity. Roughly every 11 years, at the height of the solar cycle, the Sun’s magnetic poles flip — on Earth, that’d be like the North and South Poles swapping places every decade — and the Sun transitions from sluggish to active and stormy.During the most active part of the cycle, known as solar maximum, the Sun can unleash immense explosions of light, energy, and solar radiation — all of which create conditions known as space weather. Space weather can affect satellites and astronauts in space, as well as communications systems — such as radio and GPS — and power grids on Earth. When the Sun is most active, space weather events become more frequent. Solar activity, such as the storm in May 2024, has led to increased aurora visibility and impacts on satellites and infrastructure in recent months.Listen to the media telecon.Read NASA's article about the news. || ",
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        {
            "id": 14599,
            "url": "https://svs.gsfc.nasa.gov/14599/",
            "result_type": "Produced Video",
            "release_date": "2024-06-03T11:00:00-04:00",
            "title": "Sun Releases 50th X flare of Solar Cycle 25, Quickly Followed by Two More",
            "description": "NASA’s Solar Dynamics Observatory captured this image of a solar flare – as seen in the bright eruption on the lower left – at 22:03 UTC on May 31, 2024. The image shows a blend of 131 Angstrom and 304 Angstrom light, subsets of extreme ultraviolet light. Credit: NASA/SDO || SDO_May31_2024_2204_131_304_2.jpg (4096x4096) [2.9 MB] || SDO_May31_2024_2204_131_304_2_searchweb.png (320x180) [83.2 KB] || SDO_May31_2024_2204_131_304_2_thm.png (80x40) [6.2 KB] || ",
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        {
            "id": 14588,
            "url": "https://svs.gsfc.nasa.gov/14588/",
            "result_type": "Produced Video",
            "release_date": "2024-05-09T09:00:00-04:00",
            "title": "May 2-10, 2024 : A Busy Week of Flares",
            "description": "Produced VideoWatch this video on the NASA Goddard YouTube channel.Music Credit: “Halos” from the album Burning Clouds. Written and produced by Lars Leonhard. https://ultimae.bandcamp.com/track/halos || 14588_FlareRecap_thumbnail.jpg (1280x720) [205.8 KB] || 14588_FlareRecap_X.mp4 (1920x1080) [138.1 MB] || 14588_FlareRecap_YT.mp4 (1920x1080) [337.5 MB] || 14588FlareRecapCaptions.en_US.srt [1.5 KB] || 14588FlareRecapCaptions.en_US.vtt [1.4 KB] || 14588_FlareRecap_ProRes.mov (1920x1080) [3.2 GB] || ",
            "hits": 138
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            "id": 14290,
            "url": "https://svs.gsfc.nasa.gov/14290/",
            "result_type": "Produced Video",
            "release_date": "2023-02-17T12:00:00-05:00",
            "title": "The Heliosphere Has Ripples!",
            "description": "NASA’s Interstellar Boundary Explorer, or IBEX mission, has helped researchers learn something new about the heliosphere – the magnetic bubble created by the Sun that we live in. It turns out, the heliosphere has ripples! These ripples also change – likely due to influences from the Sun itself.The paper explaining the results was published in Nature Astronomy. || ",
            "hits": 125
        },
        {
            "id": 4907,
            "url": "https://svs.gsfc.nasa.gov/4907/",
            "result_type": "Visualization",
            "release_date": "2021-06-18T11:00:00-04:00",
            "title": "A Big Sunspot from Solar Cycle 24",
            "description": "A large sunspot rotates across the view in SDO/HMI || BigSunspot_HMIintensity_stand.HD1080i.00300_print.jpg (1024x576) [50.6 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_searchweb.png (320x180) [21.8 KB] || BigSunspot_HMIintensity_stand.HD1080i.00300_thm.png (80x40) [2.6 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || BigSunspot_HMIintensity.HD1080i_p30.mp4 (1920x1080) [29.1 MB] || BigSunspot_HMIintensity.HD1080i_p30.webm (1920x1080) [2.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || BigSunspot_HMIintensity.UHD2160_p30.mp4 (3840x2160) [171.4 MB] || BigSunspot_HMIintensity.HD1080i_p30.mp4.hwshow [201 bytes] || ",
            "hits": 85
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        {
            "id": 13776,
            "url": "https://svs.gsfc.nasa.gov/13776/",
            "result_type": "Produced Video",
            "release_date": "2020-12-15T21:00:00-05:00",
            "title": "2020 AGU Roundtable: What will we learn from Solar Cycle 25?",
            "description": "Solar Cycle 25 is here, ushering in the next season of space weather from the Sun. As our star’s activity ramps up—a natural part of its roughly 11-year cycle—scientists are eager to test their predictions. In this AGU 2020 media roundtable, scientists will discuss outstanding questions in solar cycle science, what opportunities this new cycle provides researchers, and how we track progress in predictions. || ",
            "hits": 90
        },
        {
            "id": 13716,
            "url": "https://svs.gsfc.nasa.gov/13716/",
            "result_type": "Produced Video",
            "release_date": "2020-09-17T13:00:00-04:00",
            "title": "The Solar Cycle As Seen From Space",
            "description": "VIDEO IN ENGLISH Watch this video on the NASA Goddard YouTube channel.The Sun is stirring from its latest slumber. As sunspots and flares, signs of a new solar cycle, bubble from the Sun’s surface, scientists are anticipating a flurry of solar activity over the next few years. Roughly every 11 years, at the height of this cycle, the Sun’s magnetic poles flip—on Earth, that’d be like the North and South Poles’ swapping places every decade—and the Sun transitions from sluggish to active and stormy. At its quietest, the Sun is at solar minimum; during solar maximum, the Sun blazes with bright flares and solar eruptions. In this video, view the Sun's disk from our space telescopes as it transitions from minimum to maximum in the solar cycle.Music credit: \"Observance\" by Andrew Michael Britton [PRS], David Stephen Goldsmith [PRS] from Universal Production Music || 13716_SolarCycleFromSpace_YouTube.01410_print.jpg (1024x576) [68.8 KB] || 13716_SolarCycleFromSpace_YouTube.01410_searchweb.png (320x180) [35.9 KB] || 13716_SolarCycleFromSpace_YouTube.01410_web.png (320x180) [35.9 KB] || 13716_SolarCycleFromSpace_YouTube.01410_thm.png (80x40) [3.8 KB] || 13716_SolarCycleFromSpace_Twitter.mp4 (1920x1080) [21.2 MB] || 13716_SolarCycleFromSpace_YouTube.webm (1920x1080) [11.0 MB] || SolarCycleAsSeenFromSpace.en_US.srt [630 bytes] || SolarCycleAsSeenFromSpace.en_US.vtt [641 bytes] || 13716_SolarCycleFromSpace_Facebook.mp4 (1920x1080) [115.2 MB] || 13716_SolarCycleFromSpace_Prores.mov (1920x1080) [1.3 GB] || 13716_SolarCycleFromSpace_YouTube.mp4 (1920x1080) [153.6 MB] || ",
            "hits": 118
        },
        {
            "id": 13714,
            "url": "https://svs.gsfc.nasa.gov/13714/",
            "result_type": "Produced Video",
            "release_date": "2020-09-15T13:00:00-04:00",
            "title": "Solar Cycle 25 Is Here. NASA, NOAA Scientists Explain What This Means",
            "description": "Solar Cycle 25 has begun. The Solar Cycle 25 Prediction Panel announced solar minimum occurred in December 2019, marking the transition into a new solar cycle. In a press event, experts from the panel, NASA, and NOAA discussed the analysis and Solar Cycle 25 prediction, and how the rise to the next solar maximum and subsequent upswing in space weather will impact our lives and technology on Earth.A new solar cycle comes roughly every 11 years. Over the course of each cycle, the star transitions from relatively calm to active and stormy, and then quiet again; at its peak, the Sun’s magnetic poles flip. Now that the star has passed solar minimum, scientists expect the Sun will grow increasingly active in the months and years to come.Understanding the Sun’s behavior is an important part of life in our solar system. The Sun’s outbursts—including eruptions known as solar flares and coronal mass ejections—can disturb the satellites and communications signals traveling around Earth, or one day, Artemis astronauts exploring distant worlds. Scientists study the solar cycle so we can better predict solar activity.Click here for the NOAA press kit.Listen to the media telecon.Participants:• Lisa Upton, Co-chair, Solar Cycle 25 Prediction Panel; Solar Physicist, Space Systems Research Corporation• Doug Biesecker, Solar Physicist, NOAA’s Space Weather Prediction Center; Co-chair, Solar Cycle 25 Prediction Panel• Elsayed Talaat, Director, Office of Projects, Planning and Analysis; NOAA’s Satellite and Information Service • Lika Guhathakurta, Heliophysicist, Heliophysics Division, NASA Headquarters • Jake Bleacher, Chief Exploration Scientist, NASA Human Exploration and Operations Mission Directorate || ",
            "hits": 309
        },
        {
            "id": 13715,
            "url": "https://svs.gsfc.nasa.gov/13715/",
            "result_type": "Produced Video",
            "release_date": "2020-09-15T13:00:00-04:00",
            "title": "How To Track The Solar Cycle",
            "description": "A new solar cycle comes roughly every 11 years. Over the course of each cycle, the Sun transitions from relatively calm to active and stormy, and then quiet again; at its peak, the Sun’s magnetic poles flip. Now that the star has passed solar minimum, scientists expect the Sun will grow increasingly active in the months and years to come.Understanding the Sun’s behavior is an important part of life in our solar system. The Sun’s outbursts—including eruptions known as solar flares and coronal mass ejections—can disturb the satellites and communications signals traveling around Earth, or one day, Artemis astronauts exploring distant worlds. Scientists study the solar cycle so we can better predict solar activity. As of 2020, the Sun has begun to shake off the sleep of minimum, which occurred in December 2019, and Solar Cycle 25 is underway. Scientists use several indicators to track solar cycle progress. || ",
            "hits": 258
        },
        {
            "id": 13706,
            "url": "https://svs.gsfc.nasa.gov/13706/",
            "result_type": "Produced Video",
            "release_date": "2020-09-11T06:00:00-04:00",
            "title": "NASA/NOAA Interview Opportunity: Space Weather live shots",
            "description": "Click here for NOAA's Solar Minimum Press Kit with downloadable imagery and b-roll.Cut b-roll for the live shots will be posted Tuesday, Sept 15 by 4:00 p.m. EST || SolarBanner5.jpg (382x2448) [463.6 KB] || SolarBanner5_print.jpg (1024x159) [164.0 KB] || SolarBanner5_searchweb.png (320x180) [93.2 KB] || SolarBanner5_thm.png (80x40) [18.1 KB] || ",
            "hits": 48
        },
        {
            "id": 13641,
            "url": "https://svs.gsfc.nasa.gov/13641/",
            "result_type": "Produced Video",
            "release_date": "2020-06-24T10:00:00-04:00",
            "title": "A Decade of Sun",
            "description": "This 10-year time lapse of the Sun at 17.1nm shows the rise and fall of the solar cycle and notable events, like transiting planets and solar eruptions. Music: \"Solar Observer\" written and produced for this video by Lars Leonhard.Credit: NASA's Goddard Space Flight Center/SDOWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year10_Poster_1080.png (1920x1080) [7.5 MB] || SDO_Year10_Poster_1080.jpg (1920x1080) [519.0 KB] || SDO_Year10_Poster_4k.jpg (3840x2160) [972.4 KB] || SDO_Year10_Poster_4k.png (3840x2160) [27.2 MB] || SDO_10_Year_Sun_1080_15mbps.mp4 (1920x1080) [6.5 GB] || SDO_Year_10_FINAL_720FB.mp4 (1280x720) [7.3 GB] || SDO_10_Year_Sun_1080_15mbps.webm (1920x1080) [482.2 MB] || SDO_10_Year_Sun_ProRes_3840x2160_24.mov (3840x2160) [191.6 GB] || SDO_10_Year_Sun_4k_100mbps.mp4 (3840x2160) [42.9 GB] || SDO_10_Year_Sun_4k_20mbps.mp4 (3840x2160) [8.7 GB] || SDO_10_Year_Sun_SRT_Captions.en_US.srt [2.7 KB] || SDO_10_Year_Sun_SRT_Captions.en_US.vtt [2.8 KB] || ",
            "hits": 433
        },
        {
            "id": 13642,
            "url": "https://svs.gsfc.nasa.gov/13642/",
            "result_type": "Produced Video",
            "release_date": "2020-06-11T10:00:00-04:00",
            "title": "11 Years Charting The Edge of The Solar System",
            "description": "Watch this video on the NASA Goddard YouTube channel.Music credits: “End of Days - Joe Mason Remix” by Connor Shambrook [BMI], Cyrus Reynolds [BMI], Flynn Hase Spence [ASCAP], Joseph Scott Mason [APRA]; “Brainstorming” by Laurent Dury [SACEM]; “Flight of the Leaf Remix” by Julie Gruss [GEMA], Laurent Dury [SAXEM]; “Ticks and Thoughts” by Laurent Dury [SACEM]; “Intimate Journey” by Laurent Vernerey [SACEM], Nicolas de Ferran [SACEM] from Universal Production MusicComplete transcript available. || 13642_IBEX11years_YouTube.00214_print.jpg (1024x576) [239.3 KB] || 13642_IBEX11years_YouTube.00214_searchweb.png (320x180) [98.0 KB] || 13642_IBEX11years_YouTube.00214_thm.png (80x40) [6.7 KB] || 13642_IBEX11years_Prores-2.mov (1920x1080) [4.2 GB] || 13642_IBEX11years_YouTube.mp4 (1920x1080) [489.0 MB] || 13642_IBEX11years_Facebook.mp4 (1920x1080) [366.4 MB] || 13642_IBEX11years_Twitter.mp4 (1920x1080) [66.4 MB] || 13642_IBEX11years_YouTube.webm (1920x1080) [33.9 MB] || IBEX11years.en_US.srt [5.8 KB] || IBEX11years.en_US.vtt [5.8 KB] || ",
            "hits": 77
        },
        {
            "id": 13579,
            "url": "https://svs.gsfc.nasa.gov/13579/",
            "result_type": "Produced Video",
            "release_date": "2020-04-15T12:00:00-04:00",
            "title": "A Kid's Guide to Making Sunspot Cookies",
            "description": "Here are some kid-friendly instructions on how to make sugar cookies that resemble the Sun.Music: \"Day Lights\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SunspotSugarCookieStill.jpg (1920x1080) [1.3 MB] || SunspotSugarCookieStill_searchweb.png (320x180) [158.7 KB] || SunspotSugarCookieStill_thm.png (80x40) [9.4 KB] || 13579_Sunspot_Sugar_Cookies_ProRes_1920x1080_24.mov (1920x1080) [2.4 GB] || 13579_Sunspot_Sugar_Cookies_Good.mp4 (1920x1080) [227.7 MB] || 13579_Sunspot_Sugar_Cookies_Best.mp4 (1920x1080) [645.4 MB] || 13579_Sunspot_Sugar_Cookies_Good.webm (1920x1080) [26.9 MB] || 13579_Sunspot_Sugar_Cookies_SRT_Captions.en_US.srt [3.8 KB] || 13579_Sunspot_Sugar_Cookies_SRT_Captions.en_US.vtt [3.8 KB] || ",
            "hits": 37
        },
        {
            "id": 13527,
            "url": "https://svs.gsfc.nasa.gov/13527/",
            "result_type": "Produced Video",
            "release_date": "2020-01-27T12:00:00-05:00",
            "title": "New Mission Will Take First Peek at Sun’s Poles",
            "description": "A new spacecraft is journeying to the Sun to snap the first pictures of the Sun’s north and south poles. Solar Orbiter, a collaboration between ESA (the European Space Agency) and NASA will have its first opportunity to launch from Cape Canaveral on Feb. 7, 2020, at 11:15 p.m. EST. Launching on a United Launch Alliance Atlas V rocket, the spacecraft will use Venus’ and Earth’s gravity to swing itself out of the ecliptic plane — the swath of space, roughly aligned with the Sun’s equator, where all planets orbit. From there, Solar Orbiter's bird’s eye view will give it the first-ever look at the Sun's poles.Read more: https://www.nasa.gov/feature/goddard/2020/new-mission-will-take-first-peek-at-sun-s-poles || ",
            "hits": 63
        },
        {
            "id": 13275,
            "url": "https://svs.gsfc.nasa.gov/13275/",
            "result_type": "Produced Video",
            "release_date": "2019-08-07T11:30:00-04:00",
            "title": "How NASA Will Protect Astronauts From Space Radiation",
            "description": "Today, the Apollo-era flares serve as a reminder of the threat of radiation exposure for technology and astronauts in space. Understanding and predicting solar eruptions is crucial for safe space exploration. Almost 50 years since those 1972 storms, the data, technology and resources available to NASA have improved, enabling advancements towards space weather forecasts and astronaut protection — key to NASA’s Artemis program to return astronauts to the Moon.",
            "hits": 686
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        {
            "id": 4002,
            "url": "https://svs.gsfc.nasa.gov/4002/",
            "result_type": "Visualization",
            "release_date": "2017-08-04T10:00:00-04:00",
            "title": "AR2665: The Lonely Sunspot of Solar Minimum",
            "description": "Full-disk view of sunspot group moving across the solar disk, AIA 171 ångstrom band. || July2017_AR2665_AIA171_stand.HD1080i.01000_print.jpg (1024x576) [53.8 KB] || AIA171 (1920x1080) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4 (1920x1080) [53.5 MB] || July2017_AR2665_AIA171.HD1080i_p30.webm (1920x1080) [8.5 MB] || July2017_AR2665_AIA171_2048p30.mp4 (2048x2048) [264.8 MB] || 171A-Frames (4096x4096) [0 Item(s)] || 171A-Time (4096x4096) [0 Item(s)] || July2017_AR2665_AIA171.HD1080i_p30.mp4.hwshow [200 bytes] || ",
            "hits": 30
        },
        {
            "id": 12500,
            "url": "https://svs.gsfc.nasa.gov/12500/",
            "result_type": "Produced Video",
            "release_date": "2017-02-11T10:00:00-05:00",
            "title": "SDO: Year 7",
            "description": "The Solar Dynamics Observatory, or SDO, has now captured nearly seven years worth of ultra-high resolution solar footage.  This time lapse shows that full run from two of SDO's instruments.  The large orange sun is visible light captured by the Helioseismic and Magnetic Imager, or HMI.  The smaller golden sun is extreme ultraviolet light from the Atmospheric Imaging Assembly, or AIA, and reveals some of the sun's atmosphere, the corona.  Both appear at one frame every 12 hours. SDO's nearly unbroken run is now long enough to watch the rise and fall of the current solar cycle.  The graph of solar activity shows the sunspot number, a measurement based on the number of individual spots and the number of sunspot groups.  In this case, the line represents a smoothed 26-day average to more clearly show the overall trend.Music: \"Web of Intrigue\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year7_Graph_Still.jpg (3840x2160) [1.2 MB] || 12500_SDO_Year_7_Good_H264_1080.m4v (1920x1080) [239.0 MB] || 12500_SDO_Year_7_1080.mov (1920x1080) [366.0 MB] || 12500_SDO_Year_7_FINAL_appletv.m4v (1280x720) [142.4 MB] || 12500_SDO_Year_7_Compatible.m4v (960x540) [98.1 MB] || 12500_SDO_Year_7_FINAL_appletv_subtitles.m4v (1280x720) [142.5 MB] || 12500_SDO_Year_7_Compatible.webm (960x540) [24.9 MB] || 12500_SDO_Year_7_ProRes_3840x2160_2997.mov (3840x2160) [12.1 GB] || 12500_SDO_Year_7_FINAL_youtube_hq.mov (3840x2160) [6.8 GB] || 12500_SDO_Year_7-Good_H264_4K.m4v (3840x2160) [1.1 GB] || 12500_SDO_Year_7_H264_4K.mov (3840x2160) [474.8 MB] || WMV_12500_SDO_Year_7_FINAL_HD.wmv (3840x2160) [2.2 GB] || 12500_SDO_Year_7_SRT_Captions.en_US.srt [1.4 KB] || 12500_SDO_Year_7_SRT_Captions.en_US.vtt [1.4 KB] || ",
            "hits": 95
        },
        {
            "id": 12390,
            "url": "https://svs.gsfc.nasa.gov/12390/",
            "result_type": "Produced Video",
            "release_date": "2016-10-17T16:00:00-04:00",
            "title": "NASA's STEREO Solar Probes 10th Anniversary Live Shots",
            "description": "B-roll that corresponds with the live shots. || B-Roll_2.00001_print.jpg (1024x576) [130.4 KB] || B-Roll_2.00001_searchweb.png (320x180) [78.8 KB] || B-Roll_2.00001_web.png (320x180) [78.8 KB] || B-Roll_2.00001_thm.png (80x40) [6.6 KB] || B-Roll.webm (1280x720) [19.6 MB] || B-Roll_2.webm (1280x720) [19.5 MB] || B-Roll_2.mov (1280x720) [3.1 GB] || ",
            "hits": 60
        },
        {
            "id": 12071,
            "url": "https://svs.gsfc.nasa.gov/12071/",
            "result_type": "Produced Video",
            "release_date": "2015-11-30T17:00:00-05:00",
            "title": "SOHO Anniversary Live Shot Page",
            "description": "B-roll for SOHO live shot || SOHO_Broadcast_broll_youtube_print.jpg (1024x576) [98.3 KB] || SOHO_Broadcast_broll_youtube_searchweb.png (320x180) [63.4 KB] || SOHO_Broadcast_broll_youtube_thm.png (80x40) [4.9 KB] || SOHO_Broadcast_broll_prores.mov (1280x720) [2.2 GB] || SOHO_Broadcast_broll_youtube.mp4 (1280x720) [250.3 MB] || SOHO_Broadcast_broll_youtube.webm (1280x720) [15.2 MB] || ",
            "hits": 46
        },
        {
            "id": 11728,
            "url": "https://svs.gsfc.nasa.gov/11728/",
            "result_type": "B-Roll",
            "release_date": "2015-01-09T00:00:00-05:00",
            "title": "DSCOVR B-Roll",
            "description": "B-Roll of DSCOVR solar panel deploy test at Goddard Space Flight Center || DSCOVR-Cleanroom-MASTER_youtube_hq_print.jpg (1024x576) [163.7 KB] || DSCOVR-Cleanroom-MASTER_youtube_hq00027_print.jpg (1024x576) [136.8 KB] || DSCOVR-Cleanroom-MASTER_youtube_hq_searchweb.png (320x180) [100.1 KB] || DSCOVR-Cleanroom-MASTER_youtube_hq_web.png (320x180) [100.1 KB] || DSCOVR-Cleanroom-MASTER_youtube_hq_thm.png (80x40) [7.1 KB] || DSCOVR-Cleanroom-MASTER_1280x720.wmv (1280x720) [61.0 MB] || DSCOVR-Cleanroom-MASTER_prores.mov (1280x720) [1.7 GB] || DSCOVR-Cleanroom-MASTER_appletv.m4v (960x540) [49.9 MB] || DSCOVR-Cleanroom-MASTER_youtube_hq.mov (1280x720) [128.4 MB] || DSCOVR-Cleanroom-MASTER_prores.webmhd.webm (1280x720) [25.6 MB] || DSCOVR-Cleanroom-MASTER_nasaportal.mov (640x360) [50.2 MB] || DSCOVR-Cleanroom-MASTER_ipod_lg.m4v (640x360) [19.5 MB] || DSCOVR-Cleanroom-MASTER_ipod_sm.mp4 (320x240) [10.4 MB] || ",
            "hits": 16
        },
        {
            "id": 30315,
            "url": "https://svs.gsfc.nasa.gov/30315/",
            "result_type": "Hyperwall Visual",
            "release_date": "2013-10-21T12:00:00-04:00",
            "title": "World of Change: Solar Activity",
            "description": "The Sun’s activity waxes and wanes as magnetic field lines that are inside the Sun periodically break through to the surface. These breakthroughs produce a pair of sunspots of opposite magnetic polarity that travel together across the face of the Sun. The heightened magnetic activity associated with sunspots can lead to solar flares, coronal mass ejections. This series of images shows ultraviolet light (left) and sunspots (right) each spring from 1999-2010. Sunspots darken the visible surface of the Sun, producing intensely bright areas. The most recent forecast from the Space Weather Prediction Center is that solar cycle 24, which began in 2008, will be of below-average intensity, and will peak in May 2013. The small changes in solar irradiance that occur during the solar cycle exert a small influence on Earth’s climate. Images acquired from the Solar and Heliospheric Observatory (SOHO) spacecraftReference: NASA’s Earth Observatory || ",
            "hits": 65
        },
        {
            "id": 11072,
            "url": "https://svs.gsfc.nasa.gov/11072/",
            "result_type": "Produced Video",
            "release_date": "2012-11-26T10:00:00-05:00",
            "title": "SDO Solar Comparison October 2010 to October 2012",
            "description": "The sun goes through a natural solar cycle approximately every 11 years. The cycle is marked by the increase and decrease of sunspots — visible as dark blemishes on the sun's surface, or photosphere. The greatest number of sunspots in any given solar cycle is designated as \"solar maximum.\" The lowest number is \"solar minimum.\" The solar cycle provides more than just increased sunspots, however. In the sun's atmosphere, or corona, bright active regions appear, which are rooted in the lower sunspots. Scientists track the active regions since they are often the origin of eruptions on the sun such as solar flares or coronal mass ejections. The most recent solar minimum occurred in 2008, and the sun began to ramp up in January 2010, with an M-class flare (a flare that is 10 times less powerful than the largest flares, labeled X-class). The sun has continued to get more active, with the next solar maximum predicted for 2013. The journey toward solar maximum is evident in current images of the sun, showing a marked difference from those of 2010, with bright active regions dotted around the star. || ",
            "hits": 58
        },
        {
            "id": 10754,
            "url": "https://svs.gsfc.nasa.gov/10754/",
            "result_type": "Produced Video",
            "release_date": "2011-11-10T00:00:00-05:00",
            "title": "The Truth About 2012: Solar Storms",
            "description": "Should we be concerned about solar storms in 2012? Heliophysicist Alex Young from NASA Goddard Space Flight Center sorts out truth from fiction. || ",
            "hits": 68
        },
        {
            "id": 10804,
            "url": "https://svs.gsfc.nasa.gov/10804/",
            "result_type": "Produced Video",
            "release_date": "2011-10-27T08:00:00-04:00",
            "title": "The Solar Cycle",
            "description": "The number of sunspots increases and decreases over time in a regular, approximately 11-year cycle, called the sunspot cycle. The exact length of the cycle can vary. It has been as short as eight years and as long as fourteen, but the number of sunspots always increases over time, and then returns to low again. More sunspots mean increased solar activity, when great blooms of radiation known as solar flares or bursts of solar material known as coronal mass ejections (CMEs) shoot off the sun's surface. The highest number of sun spots in any given cycle is designated \"solar maximum,\" while the lowest number is designated \"solar minimum.\" Each cycle, varies dramatically in intensity, with some solar maxima being so low as to be almost indistinguishable from the preceding minimum. Sunspots are a magnetic phenomenon and the entire sun is magnetized with a north and a south magnetic pole just like a bar magnet. The comparison to a simple bar magnet ends there, however, as the sun's interior is constantly on the move. By tracking sound waves that course through the center of the sun, an area of research known as helioseismology, scientists can gain an understanding of what's deep inside the sun. They have found that the magnetic material inside the sun is constantly stretching, twisting, and crossing as it bubbles up to the surface. The exact pattern of movements is not conclusively mapped out, but over time they eventually lead to the poles reversing completely. The sunspot cycle happens because of this poles flip — north becomes south and south becomes north—approximately every 11 years. Some 11 years later, the poles reverse again back to where they started, making the full solar cycle actually a 22-year phenomenon. The sun behaves similarly over the course of each 11-year cycle no matter which pole is on top, however, so this shorter cycle tends to receive more attention. || ",
            "hits": 606
        },
        {
            "id": 10109,
            "url": "https://svs.gsfc.nasa.gov/10109/",
            "result_type": "Produced Video",
            "release_date": "2011-08-09T10:00:00-04:00",
            "title": "X-Class: A Guide to Solar Flares",
            "description": "Flares happen when the powerful magnetic fields in and around the sun reconnect. They're usually associated with active regions, often seen as sun spots, where the magnetic fields are strongest. Flares are classified according to their strength. The smallest ones are B-class, followed by C, M and X, the largest. Similar to the Richter scale for earthquakes, each letter represents a ten-fold increase in energy output. So an X is 10 times an M and 100 times a C. Within each letter class, there is a finer scale from 1 to 9. C-class flares are too weak to noticeably affect Earth. M-class flares can cause brief radio blackouts at the poles and minor radiation storms that might endanger astronauts. Although X is the last letter, there are flares more than 10 times the power of an X1, so X-class flares can go higher than 9. The most powerful flare on record was in 2003, during the last solar maximum. It was so powerful that it overloaded the sensors measuring it. They cut-out at X17, and the flare was later estimated to be about X45. A powerful X-class flare like that can create long lasting radiation storms, which can harm satellites and even give airline passengers, flying near the poles, small radiation doses. X flares also have the potential to create global transmission problems and world-wide blackouts. || ",
            "hits": 2784
        },
        {
            "id": 20185,
            "url": "https://svs.gsfc.nasa.gov/20185/",
            "result_type": "Animation",
            "release_date": "2010-10-01T11:00:00-04:00",
            "title": "Heliopause Cycle",
            "description": "This animation shows the heliosphere expanding and contracting in response to the solar cycle. As the sun reaches solar maximum, the solar wind increases and expands the heliosphere. During solar minimum, the heliosphere contracts. || ",
            "hits": 72
        },
        {
            "id": 10411,
            "url": "https://svs.gsfc.nasa.gov/10411/",
            "result_type": "Produced Video",
            "release_date": "2009-03-18T00:00:00-04:00",
            "title": "The Top 5 Solar Discoveries",
            "description": "A countdown of the top 5 solar discoveries from the Sun-Earth Connection Education Forum. These include the discoveries of sunspots, the solar cycle, the heliosphere, aurora formation, and space weather. || ",
            "hits": 59
        },
        {
            "id": 10396,
            "url": "https://svs.gsfc.nasa.gov/10396/",
            "result_type": "Produced Video",
            "release_date": "2009-02-19T00:00:00-05:00",
            "title": "Solar Variability and Total Solar Irradiance (TSI)",
            "description": "Analyzing the Sun and its effects on climate is complicated by the fact that the amount of radiation arriving from the Sun is not constant. It varies from the average value of the total solar irradiance (TSI)—1,361 W/m2—on a daily basis. Variations in TSI are due to a balance between decreases caused by sunspots and increases caused by faculae, which are the bright areas that surround sunspots. The Sun's energy output varies with time, and Glory's TIM instrument will help measure those fluctuations by continued monitoring of TSI. Data from TIM will extend the long-term climate record, which has been uninterrupted since 1978 and provides the best estimate available of solar inputs to climate. This short movie displays the Sun rotating and the corresponding total solar irradiance. || ",
            "hits": 575
        },
        {
            "id": 3566,
            "url": "https://svs.gsfc.nasa.gov/3566/",
            "result_type": "Visualization",
            "release_date": "2008-12-18T00:00:00-05:00",
            "title": "Multi-Sun Composition",
            "description": "This movie is a composition of multiple solar datasets synchronized in time. The time frame is late October and early November of 2003, the time of some record-breaking solar activity.The background of the movie shows the view of the wide-angle coronagraphs (blue/white), or LASCO instruments, aboard SOHO. They show streams of electrons outbound from the Sun, part of the solar atmosphere. The central green image is the Sun in ultraviolet light from the EIT instrument. Note that flashes of solar flares in the ultraviolet quickly propagate out from the Sun and are visible in LASCO. These events are coronal mass ejections, or CMEs.Overlaid on the upper left is a better view of the EIT ultraviolet image at a wavelength of 195 angstroms (19.5 nanometers).On the lower left, the orange movie is the EIT ultraviolet movie at 304 angstroms (30.4 nanometers).On the upper right is a solar magnetogram, taken by the MDI instrument. The white regions correspond to positive (north) magnetic flux and the dark regions to negative (south) magnetic flux.The colors for the sequences above are not real. They are chosen by convention since the properties recorded by the cameras are not visible to the human eye.The final image on the lower right is also from MDI. It is a combination of several optical wavelengths and is the best representation from SOHO of the Sun in visible light, as we would see it through ground-based telescopes.The movies that are part of this composition are also available individually on the SVS site: Halloween Solar Storms 2003: SOHO/EIT and SOHO/LASCOHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 195 angstromsHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 304 angstromsHalloween Solar Storms 2003: SOHO/MDI ContinuumHalloween Solar Storms 2003: SOHO/MDI Magnetograms || ",
            "hits": 30
        },
        {
            "id": 3496,
            "url": "https://svs.gsfc.nasa.gov/3496/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Plasma Flows",
            "description": "In this visualization, we illustrate the fluid flows in the Sun which drive the solar magnetic dynamo. The flows can be considered as a combination of two components, a toroidal component and a meridional component. The toroidal flow corresponds to the rotational motion of the Sun. In the cut-away view, this motion is represented by the streaking flow vectors. The color code of the cross-section on the right-hand side illustrates the rotational period of this flow. Here we see that flow near the equator (in violet) takes about 24.5 days to make it all the way around the Sun. As we move to higher latitudes, we see that the flow gets steadily slower, increasing the time it takes to go around the Sun to as much as 34 days (in red) near the poles. A non-uniform fluid flow such as this is known as differential rotation. This motion in the interior can be measured at the solar surface through techniques of helioseismology.Deeper into the Sun, we see the different colors of the outer layers transition to a solid color (olive green). This transition point is called the tachocline. It is the boundary between the outer zone of the Sun where thermal energy is transferred by convection (the convective zone), and the inner region of the Sun where thermal energy is transferred by radiation (the radiative zone). The radiative zone is believed to rotate as a solid body with a period of about 28 days in this model.The yellow and white center in this model represents the solar radiative zone.In the cross-section on the left-side, we represent the other component of the flow, called the meridional flow, which moves plasma between the equator and the polar regions.These flows of solar plasma are used as input data for dynamo modeling (see The Solar Dynamo: Toroidal and Poloidal Fields and The Solar Dynamo: Toroidal and Radial Fields.) || ",
            "hits": 117
        },
        {
            "id": 3521,
            "url": "https://svs.gsfc.nasa.gov/3521/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Toroidal and Poloidal Magnetic Fields",
            "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, the field intensity represented by colors on the right-hand cross-section, and the poloidal magnetic potential field, represented by colors on the left-hand cross-section. The poloidal magnetic potential is a scalar quantity that contains information about the radial and latitudinal magnetic field vectors. To see the radial magnetic field, see The Solar Dynamo: Toroidal and Radial Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time. Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field. Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator as the solar cycle progresses. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ",
            "hits": 128
        },
        {
            "id": 3583,
            "url": "https://svs.gsfc.nasa.gov/3583/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Toroidal and Radial Magnetic Fields",
            "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, intensities represented by color on the right-hand cross-section, and the radial magnetic field, represented on the left-hand cross-section. To see the poloidal magnetic vector potential, see The Solar Dynamo: Toroidal and Poloidal Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time.Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field.Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ",
            "hits": 102
        },
        {
            "id": 20156,
            "url": "https://svs.gsfc.nasa.gov/20156/",
            "result_type": "Animation",
            "release_date": "2008-07-21T12:00:00-04:00",
            "title": "Solar - B (Hinode) Spacecraft",
            "description": "Solar - B Spacecraft goes into orbit to begin looking at the sun. It is specifically looking at solar magnetic fields and the origins of the solar wind. || ",
            "hits": 24
        },
        {
            "id": 20133,
            "url": "https://svs.gsfc.nasa.gov/20133/",
            "result_type": "Animation",
            "release_date": "2008-02-21T00:00:00-05:00",
            "title": "Solar Cycle (High Definition)",
            "description": "This animation shows sunpot migration over a 11 year solar cycle and indicates the features causing total solar irradiance variability. For a standard definition version of this animation, please go to animation 10151. || ",
            "hits": 55
        },
        {
            "id": 2921,
            "url": "https://svs.gsfc.nasa.gov/2921/",
            "result_type": "Visualization",
            "release_date": "2005-03-08T12:00:00-05:00",
            "title": "Solar Tsunamis",
            "description": "Push-in to a region of the Sun to witness a 'solar tsunami' after a flare event.  The tsunami moves hot gas (bright) out of the region, revealing cooler regions (darker) below. || ",
            "hits": 47
        },
        {
            "id": 2922,
            "url": "https://svs.gsfc.nasa.gov/2922/",
            "result_type": "Visualization",
            "release_date": "2005-03-08T12:00:00-05:00",
            "title": "Solar Tsunamis - View with a Spin",
            "description": "Push-in to a region of the Sun to witness a 'solar tsunami' after a flare event.  The tsunami moves hot gas (bright) out of the region, revealing cooler regions (darker) below.  This view rotates on the push-in to keep the region of the flare event visible (to the left in the final frame). || ",
            "hits": 11
        },
        {
            "id": 2936,
            "url": "https://svs.gsfc.nasa.gov/2936/",
            "result_type": "Visualization",
            "release_date": "2004-05-23T12:00:00-04:00",
            "title": "The fastest CME of Cycle 23 overtakes another fast CME",
            "description": "On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft. || ",
            "hits": 71
        },
        {
            "id": 2856,
            "url": "https://svs.gsfc.nasa.gov/2856/",
            "result_type": "Visualization",
            "release_date": "2003-11-11T12:00:00-05:00",
            "title": "Model of the Heliosphere Over the Solar Cycle",
            "description": "This magnetohydrodynamical (MHD) model shows how the heliosphere of the Sun might interact with the local interstellar medium (ISM) over the course of a single 11 year solar cycle.  The sun (and the orbit of the Earth) is located in the tiny blue region in the center.  The ISM is moving from left to right.  The solar wind varies from 400 km/s up to 566 km/s and back down to 400 km/s over the cycle in this particular model.  The colors are logarithmically scaled to represent temperature, with blue around 10,000 Kelvins (in the undisturbed ISM and the region immediately around the Sun) and red over 1,000,000 Kelvins (corresponding to the bow shocked region in the plasma).  The green region around the Sun has a radius that varies between 100-200 Astronomical Units. || ",
            "hits": 70
        },
        {
            "id": 2644,
            "url": "https://svs.gsfc.nasa.gov/2644/",
            "result_type": "Visualization",
            "release_date": "2003-01-02T12:00:00-05:00",
            "title": "The Solar 'Constant' - Faculae vs. Sunspots",
            "description": "Three views of the Sun showing different levels of solar activity. The color table has been altered to enhance the appearance of the faculae (white regions) which are hotter than sunspots (red-black regions) and whose greater total area contribute to increasing the solar flux reaching the Earth. || Low solar activity - October 28, 1998 || activity-01-low.jpg (2048x2048) [437.9 KB] || activity-01-low_web.jpg (320x320) [21.2 KB] || activity-01-low.tif (2048x2048) [1.7 MB] || ",
            "hits": 51
        }
    ]
}