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    "results": [
        {
            "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": 498
        },
        {
            "id": 14530,
            "url": "https://svs.gsfc.nasa.gov/14530/",
            "result_type": "Produced Video",
            "release_date": "2024-02-21T08:00:00-05:00",
            "title": "Goldstone Apple Valley Radio Telescope (GAVRT) Solar Patrol",
            "description": "The Goldstone Apple Valley Radio Telescope (GAVRT) is located in Goldstone, California. It is a reconfigured antenna used for teaching purposes.The GAVRT program teaches K-12 students how to calibrate this 34-meter antenna (known as Deep Space Station-28), collect and distribute science data through the Internet and get excited about radio astronomy. Students collaborate with scientists who are working on the same mission and are recognized as part of the science team. Data collected and analyzed by the students is used by NASA in their studies of the solar system.During the April 8, 2024, total solar eclipse, NASA’s Jet Propulsion Laboratory, educators at the Lewis Center for Education Research in Southern California, and participants in the center’s Solar Patrol citizen science program will observe solar “active regions” – the magnetically complex regions that form over sunspots – as the Moon moves over them. The Moon’s gradual passage across the Sun blocks different portions of the active region at different times, allowing scientists to distinguish light signals coming from one portion versus another. The technique, first used during the May 2012 annular eclipse, revealed details on the Sun the telescope couldn’t otherwise detect. || ",
            "hits": 90
        },
        {
            "id": 4892,
            "url": "https://svs.gsfc.nasa.gov/4892/",
            "result_type": "Visualization",
            "release_date": "2022-01-18T12:00:00-05:00",
            "title": "Faculae and Sunspots at Solar Maximum and Solar Minimum",
            "description": "Movie of SDO/AIA 1700 angstrom imagery, collected near solar maximum (April 2014).  Note the small dark regions (sunspots) and the brighter speckled regions (faculae) around them. || SolarMax_AIA1700A_stand.HD1080i.00300_print.jpg (1024x576) [61.4 KB] || SolarMax_AIA1700A_stand.HD1080i.00300_searchweb.png (320x180) [35.9 KB] || SolarMax_AIA1700A_stand.HD1080i.00300_thm.png (80x40) [3.3 KB] || SolarMax_AIA1700A (1920x1080) [0 Item(s)] || SolarMax_AIA1700A_stand.HD1080i_p30.mp4 (1920x1080) [66.8 MB] || SolarMax_AIA1700A_stand.HD1080i_p30.webm (1920x1080) [3.0 MB] || SolarMax_AIA1700A (3840x2160) [0 Item(s)] || SolarMax_AIA1700A_stand.UHD2160_p30.mp4 (3840x2160) [270.8 MB] || SolarMax_AIA1700A_stand.HD1080i_p30.mp4.hwshow [201 bytes] || ",
            "hits": 87
        },
        {
            "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": 71
        },
        {
            "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": 109
        },
        {
            "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": 305
        },
        {
            "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": 34
        },
        {
            "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": 279
        },
        {
            "id": 4715,
            "url": "https://svs.gsfc.nasa.gov/4715/",
            "result_type": "Visualization",
            "release_date": "2019-06-07T00:00:00-04:00",
            "title": "Swedish Solar Telescope: Solar Closeups",
            "description": "Close-up of Active Region 12593 through the 400 nm filter of the Swedish Solar Telescope.  SDO/HMI provides the background image. || Sept2016_CHROMIS4000A_stand.HD1080i.00100_print.jpg (1024x576) [200.8 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_searchweb.png (180x320) [136.4 KB] || Sept2016_CHROMIS4000A_stand.HD1080i.00100_thm.png (80x40) [9.1 KB] || SwedishST (1920x1080) [0 Item(s)] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4 (1920x1080) [19.4 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.webm (1920x1080) [1.5 MB] || SwedishST (3840x2160) [0 Item(s)] || Sept2016_CHROMIS4000A.UHD3840_2160p30.mp4 (3840x2160) [50.6 MB] || Sept2016_CHROMIS4000A.HD1080i_p30.mp4.hwshow [199 bytes] || ",
            "hits": 132
        },
        {
            "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": 51
        },
        {
            "id": 12105,
            "url": "https://svs.gsfc.nasa.gov/12105/",
            "result_type": "Produced Video",
            "release_date": "2017-08-04T09:00:00-04:00",
            "title": "Two Weeks in the Life of a Sunspot",
            "description": "Watch this video on the NASA Goddard YouTube channel.Complete transcript available.Music credit: Foraging at Dusk by Benjamin James Parsons || sunspotthumb1_print.jpg (1024x576) [139.0 KB] || sunspotthumb1.jpg (1920x1080) [144.7 KB] || sunspotthumb1_thm.png (80x40) [8.2 KB] || sunspotthumb1_web.png (320x180) [137.9 KB] || sunspotthumb1_searchweb.png (320x180) [137.9 KB] || APPLE_TV-12105_Life_of_a_SunspotV5_appletv.m4v (1280x720) [56.1 MB] || 12105_Life_of_a_SunspotV5.webm (1920x1080) [12.4 MB] || APPLE_TV-12105_Life_of_a_SunspotV5_appletv_subtitles.m4v (1280x720) [56.1 MB] || FACEBOOK_720-12105_Life_of_a_SunspotV5_facebook_720.mp4 (1280x720) [131.6 MB] || LARGE_MP4-12105_Life_of_a_SunspotV5_large.mp4 (1920x1080) [114.4 MB] || YOUTUBE_1080-12105_Life_of_a_SunspotV5_youtube_1080.mp4 (1920x1080) [180.9 MB] || NASA_TV-12105_Life_of_a_SunspotV5.mpeg (1280x720) [377.0 MB] || YOUTUBE_HQ-12105_Life_of_a_SunspotV5_youtube_hq.mov (1920x1080) [805.0 MB] || PRORES_B-ROLL-12105_Life_of_a_SunspotV5_prores.mov (1280x720) [787.9 MB] || lifeofasunspotV5.en_US.vtt [1.3 KB] || lifeofasunspotV5.en_US.srt [1.3 KB] || 12105_Life_of_a_SunspotV5.mov (1920x1080) [1.5 GB] || NASA_PODCAST-12105_Life_of_a_SunspotV5_ipod_sm.mp4 (320x240) [19.1 MB] || 12105_Life_of_a_SunspotV5_lowres.mp4 (480x272) [15.4 MB] || ",
            "hits": 44
        },
        {
            "id": 12613,
            "url": "https://svs.gsfc.nasa.gov/12613/",
            "result_type": "Produced Video",
            "release_date": "2017-06-02T11:00:00-04:00",
            "title": "SDO 4k Slow-rotation Sun Resource Page",
            "description": "Still Image for page || SDO_Slow_Gallery.jpg (1920x1080) [235.4 KB] || SDO_Slow_Gallery_searchweb.png (320x180) [43.0 KB] || SDO_Slow_Gallery_thm.png (80x40) [3.6 KB] || ",
            "hits": 173
        },
        {
            "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": 75
        },
        {
            "id": 11720,
            "url": "https://svs.gsfc.nasa.gov/11720/",
            "result_type": "Produced Video",
            "release_date": "2014-11-20T00:00:00-05:00",
            "title": "Sunspot Live Shots 2014",
            "description": "Canned interviews for Sunspot live shot 11/20/2014 || Alex_Young_Canned_interview_youtube_hq_print.jpg (1024x576) [102.0 KB] || Alex_Young_Canned_interview_youtube_hq_web.png (320x180) [86.5 KB] || Alex_Young_Canned_interview_youtube_hq_thm.png (80x40) [6.8 KB] || Alex_Young_Canned_interview_appletv.m4v (960x540) [86.6 MB] || Alex_Young_Canned_interview_appletv.webmhd.webm (960x540) [40.6 MB] || Alex_Young_Canned_interview_appletv_subtitles.m4v (960x540) [86.7 MB] || Alex_Young_Canned_interview_1280x720.wmv (1280x720) [106.0 MB] || Alex_Young_Canned_interview_youtube_hq.mov (1280x720) [289.0 MB] || Alex_Young_Canned_interview_ipod_lg.m4v (640x360) [34.0 MB] || Alex_Young_Canned_Interview.en_US.srt [4.0 KB] || Alex_Young_Canned_Interview.en_US.vtt [4.0 KB] || Alex_Young_Canned_interview_nasaportal.mov (640x360) [86.1 MB] || Alex_Young_Canned_interview_ipod_sm.mp4 (320x240) [18.0 MB] || Alex_Young_Canned_interview_prores.mov (1280x720) [3.1 GB] || ",
            "hits": 32
        },
        {
            "id": 11460,
            "url": "https://svs.gsfc.nasa.gov/11460/",
            "result_type": "Produced Video",
            "release_date": "2014-02-11T12:00:00-05:00",
            "title": "SDO: Year 4",
            "description": "The sun is always changing and NASA's Solar Dynamics Observatory is always watching. Launched on Feb. 11, 2010, SDO keeps a 24-hour eye on the entire disk of the sun, with a prime view of the graceful dance of solar material coursing through the sun's atmosphere, the corona. SDO's fourth year in orbit was no exception: NASA is releasing a movie of some of SDO's best sightings of the year, including massive solar explosions and giant sunspot shows. SDO captures images of the sun in 10 different wavelengths, each of which helps highlight a different temperature of solar material. Different temperatures can, in turn, show specific structures on the sun such as solar flares, which are giant explosions of light and x-rays, or coronal loops, which are streams of solar material traveling up and down looping magnetic field lines. The movie shows examples of both, as well as what's called prominence eruptions, when masses of solar material leap off the sun. The movie also shows a sunspot group on the solar surface. This sunspot, a magnetically strong and complex region appearing in mid-January 2014, was one of the largest in nine years. Scientists study these images to better understand the complex electromagnetic system causing the constant movement on the sun, which can ultimately have an effect closer to Earth, too: Flares and another type of solar explosion called coronal mass ejections can sometimes disrupt technology in space. Moreover, studying our closest star is one way of learning about other stars in the galaxy. NASA's Goddard Space Flight Center in Greenbelt, Md. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.SDO: Year One here.SDO: Year 2 here.SDO: Year 3 here.Information about the individual clips used in this video is here. || ",
            "hits": 115
        },
        {
            "id": 4133,
            "url": "https://svs.gsfc.nasa.gov/4133/",
            "result_type": "Visualization",
            "release_date": "2014-02-11T10:00:00-05:00",
            "title": "February 2013: The Busy Sun",
            "description": "Even near solar maximum, with sunspots dotting the photosphere, the Sun can look tranquil and serene in visible light. In the case of these images from the HMI instrument on the Solar Dynamics Observatory, the only obvious changes are the constant shimmering of the solar disk due to the bubbling of solar granulation.But in ultraviolet light, in particular the 30.4 nanometer line of the helium ion, we see much more activity. Dark, wispy lines of cooler solar filaments (the term used for solar prominences when seen against the disk) stretch across the disk. The same structures, seen against the fainter glow of the solar corona, resemble slowly evolving flames on the limb of the Sun. Solar active regions surrounding the sunspots, appear bright in ultraviolet light. || ",
            "hits": 44
        },
        {
            "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": 63
        },
        {
            "id": 4061,
            "url": "https://svs.gsfc.nasa.gov/4061/",
            "result_type": "Visualization",
            "release_date": "2013-04-16T00:00:00-04:00",
            "title": "Solar Close-ups with Hinode's Solar Optical Telescope",
            "description": "A collection of movies generated from the Solar Optical Telescope (SOT) of the JAXA/NASA Hinode mission. || ",
            "hits": 42
        },
        {
            "id": 11211,
            "url": "https://svs.gsfc.nasa.gov/11211/",
            "result_type": "Produced Video",
            "release_date": "2013-02-22T10:00:00-05:00",
            "title": "SDO Observes Fast-Growing Sunspot",
            "description": "As magnetic fields on the sun rearrange and realign, dark spots known as sunspots can appear on its surface. Over the course of Feb. 19-20, 2013, scientists watched a giant sunspot form in under 48 hours. It has grown to over six Earth diameters across but its full extent is hard to judge since the spot lies on a sphere not a flat disk.The spot quickly evolved into what's called a delta region, in which the lighter areas around the sunspot, the penumbra, exhibit magnetic fields that point in the opposite direction of those fields in the center, dark area. This is a fairly unstable configuration that scientists know can lead to eruptions of radiation on the sun called solar flares. || ",
            "hits": 99
        },
        {
            "id": 4037,
            "url": "https://svs.gsfc.nasa.gov/4037/",
            "result_type": "Visualization",
            "release_date": "2013-02-11T10:00:00-05:00",
            "title": "Sunspot Growth in June 2012",
            "description": "Groups of sunspots grow and die over a matter of days. This is a movie built from images taken by the SDO/HMI instrument over the course of 13 days during the rise of solar cycle 24. || ",
            "hits": 37
        },
        {
            "id": 3897,
            "url": "https://svs.gsfc.nasa.gov/3897/",
            "result_type": "Visualization",
            "release_date": "2012-01-27T00:00:00-05:00",
            "title": "Growing Sunspots - A Full Disk View: February 2011",
            "description": "Here is a leisurely view of SDO/HMI data, sampled every hour, covering two weeks in the middle of February 2011. While the solar disk starts out featureless, eventually small groups of sunspots (the darker regions) emerge, grow, and then rotate out of view.For a closeup view of of one of these sunspot groups, see animation 3898, Growing Sunspots - Tracking Closeup: February 2011 || ",
            "hits": 52
        },
        {
            "id": 3898,
            "url": "https://svs.gsfc.nasa.gov/3898/",
            "result_type": "Visualization",
            "release_date": "2012-01-27T00:00:00-05:00",
            "title": "Growing Sunspots - Tracking Closeup: February 2011",
            "description": "This visualization tracks the emergence and evolution of a sunspot group as seen by SDO/HMI starting in early February 2011 and continuing for two weeks. Images are sampled one hour apart.In this version, the camera tracks the movement of the solar rotation.At this scale, a 'shimmer' of the solar surface is visible, created by the turnover of convection cells. A higher-resolution view of these convection cells can be seen in Hinode imagery (see entry #3412, Hinode's High-resolution view of solar granulation).For a full-disk view of the Sun, covering the same time frame, see entry #3897, Growing Sunspots - A Full Disk View: February 2011. || ",
            "hits": 37
        },
        {
            "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": 518
        },
        {
            "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": 2247
        },
        {
            "id": 10718,
            "url": "https://svs.gsfc.nasa.gov/10718/",
            "result_type": "Produced Video",
            "release_date": "2011-02-06T10:00:00-05:00",
            "title": "STEREO Sun360",
            "description": "Launched in October 2006, STEREO traces the flow of energy and matter from the sun to Earth. It also provides unique and revolutionary views of the sun-Earth system. The mission observed the sun in 3-D for the first time in 2007. In 2009, the twin spacecraft revealed the 3-D structure of coronal mass ejections which are violent eruptions of matter from the sun that can disrupt communications, navigation, satellites and power grids on Earth.Seeing?the whole sun front and back simultaneously will enable significant advances in space weather forecasting for Earth and for planning for future robotic and manned spacecraft missions throughout the solar system.These views are the result of observations by NASA's two Solar TErrestrial Relations Observatory (STEREO) spacecraft. The duo are on diametrically opposite sides of the sun, 180 degrees apart. One is ahead of Earth in its orbit, the other trailing behind.For the STEREO Sun360 Teaser, go here.For the full visualization showing STEREO's path go here.For the visualization showing STEREO's increasing coverage of the sun (visual 3) go here.For animations from the STEREO Teaser and stages of coverage, go here.For animations showing STEREO's 3D coverage of a CME go here. || ",
            "hits": 218
        },
        {
            "id": 3794,
            "url": "https://svs.gsfc.nasa.gov/3794/",
            "result_type": "Visualization",
            "release_date": "2010-11-09T00:00:00-05:00",
            "title": "STEREO in Stereo: April 8, 2007",
            "description": "Full Disk View: Image sequences taken April 8-9, 2007 by the EUVI telescopes on the two STEREO spacecraft (STEREO-B, left eye; STEREO-A, right eye). At this time the spacecraft were about 3.7 degrees apart. These images show the Sun in extreme ultraviolet light at a wavelength of 171 angstroms, highlighting parts of the Sun's atmosphere (the corona) at about one million degrees C. Note the bright active regions near the Sun's equator and the dark \"coronal holes\" at the north and south poles. These are features of the Sun's magnetic field. Coronal holes are areas where the magnetic field opens out to allow material to flow out into the solar system, while active regions are made up of strong, closed fields which bottle up hot plasma (ionized gas) close to the surface. This image was taken near the minimum in solar activity, so there are few active regions.Closeup View: Image sequences taken April 8-9, 2007 by the EUVI telescopes in the SECCHI imaging suites on the two STEREO spacecraft (STEREO-B, left eye; STEREO-A, right eye). At this time the spacecraft were about 3.7 degrees apart. Here we see a close up of solar magnetic active regions, flickering as they rotate out of sight around the sun. These are areas where the Sun's strong magnetic field bottles up million degree C plasma (ionized gas) low in the corona (the Sun's outer atmosphere). These images are taken at a wavelength of 171 angstroms (0.00000171 cm) in the extreme ultraviolet.Note for Large Displays: These movies are produced using images from STEREO where the angle between the spacecraft is getting larger than the optimum angle for stereo separation. While they work well on small displays, large-screens and projection systems can introduce significant distortions in the stereo effect which the audience may find uncomfortable. When doing large-screen projection, you may need to adjust the left-right image alignment for optimum viewing. However, this does not guarantee a distortion-free result. || ",
            "hits": 36
        },
        {
            "id": 3695,
            "url": "https://svs.gsfc.nasa.gov/3695/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/AIA CME Event of April 8, 2010 Full Disk (Multiband)",
            "description": "This visualization is a full-disk view of the CME launched from the Sun on April 8, 2010. This is a 3-color image produced by combining three different filters from the AIA instrument: 211 (red), 193 (green), and 171 (blue). || ",
            "hits": 29
        },
        {
            "id": 3696,
            "url": "https://svs.gsfc.nasa.gov/3696/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Continuum Full Disk View - March 29, 2010",
            "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ",
            "hits": 40
        },
        {
            "id": 3703,
            "url": "https://svs.gsfc.nasa.gov/3703/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Continuum Sunspot Closeup - March 29, 2010",
            "description": "This is a close-up view of a large sunspot group visible as the HMI instrument turned on their imagers. || ",
            "hits": 14
        },
        {
            "id": 3704,
            "url": "https://svs.gsfc.nasa.gov/3704/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Continuum Sunspot Zoom-in - March 29, 2010",
            "description": "This is a zoom-in view of a large sunspot group visible as the HMI instrument turned on their imagers. || ",
            "hits": 32
        },
        {
            "id": 3705,
            "url": "https://svs.gsfc.nasa.gov/3705/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Sunspot Close-Up - March 29, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This version is a close-up view of a large sunspot group. || ",
            "hits": 26
        },
        {
            "id": 3706,
            "url": "https://svs.gsfc.nasa.gov/3706/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Sunspot Zoom-In - March 29, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This movie zooms-in on a large sunspot group. || ",
            "hits": 34
        },
        {
            "id": 3712,
            "url": "https://svs.gsfc.nasa.gov/3712/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Continuum Full Disk View - April 7, 2010",
            "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ",
            "hits": 61
        },
        {
            "id": 3713,
            "url": "https://svs.gsfc.nasa.gov/3713/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Full Disk View - April 7, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Gray is zero magnetic field.Notice that the surface magnetic fields reveal much more structure than the white-light images in SDO/HMI Continuum Full Disk View - April 7, 2010. || ",
            "hits": 22
        },
        {
            "id": 3714,
            "url": "https://svs.gsfc.nasa.gov/3714/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Dopplergram Sunspot Close-Up - March 29, 2010",
            "description": "The dopplergram from SDO/HMI data shows the velocity of solar material on the line-of-sight. White pixels are moving away from the camera and black pixels are moving towards the camera. || ",
            "hits": 48
        },
        {
            "id": 3716,
            "url": "https://svs.gsfc.nasa.gov/3716/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/AIA Full-Disk View of Launching Filament (Band 304)",
            "description": "Full disk view of a filament launch in the SDO AIA 304 band. || ",
            "hits": 53
        },
        {
            "id": 3691,
            "url": "https://svs.gsfc.nasa.gov/3691/",
            "result_type": "Visualization",
            "release_date": "2010-03-31T00:00:00-04:00",
            "title": "A Comparative View of the Sun: SDO/AIA 193 and SOHO/EIT 195",
            "description": "This movie compares the spatial and temporal resolutions of the SDO/AIA (Atmospheric Imaging Assembly) imager to the SOHO/EIT (Extreme ultraviolet Imaging Telescope) imager. SOHO/EIT's highest resolution is 1024x1024 pixels with images taken about every 12 minutes for the 195 Ångstrom band. The SDO/AIA 193 band takes images at 4096x4096 pixels every twelve seconds!In this movie we can see the difference this makes for a closeup view of Active Region 1087. EIT reveals changes in the active region, which AIA reveals many details.This visualization is a companion piece to A Comparative View of the Sun: SDO/AIA 193 and STEREO-B/EUVI 195. || ",
            "hits": 77
        },
        {
            "id": 10584,
            "url": "https://svs.gsfc.nasa.gov/10584/",
            "result_type": "Produced Video",
            "release_date": "2010-03-22T00:00:00-04:00",
            "title": "Heliophysics Program Overview",
            "description": "This short program overview for NASA's heliophysics division explains how NASA studies the sun—and more importantly—how it affects our daily lives. || ",
            "hits": 66
        },
        {
            "id": 10583,
            "url": "https://svs.gsfc.nasa.gov/10583/",
            "result_type": "Produced Video",
            "release_date": "2010-03-16T00:00:00-04:00",
            "title": "Slices Through the Solar Interior",
            "description": "Scientists using SOHO/MDI data have looked just below the Sun's surface and clearly observed inward flowing material.The strong magnetic fields in the sunspots promote cooling. Cool material contracts and sinks at speeds of up to 3000 miles per hour. This drives an inward flow, like a planet-sized whirlpool, that holds the sunspot together as long as the field is strong enough. Scientists discovered this using a technique called acoustic tomography - a novel method similar to ultrasound diagnostics in medicine that uses sound waves to image structures inside the human body. Scientists also found that sunspots are surprisingly shallow. Conditions in sunspots change from cooler than the surrounding plasma to hotter than the surrounding plasma just 3000 miles below the surface. The cool part of a sunspot has the shape of a stack of two or three nickels. Sunspot magnetic fields block the flows that carry heat energy up from the hot solar interior. That results in higher temperatures below the blockage and cooler temperatures above. The downward flows mentioned above dissipate at the same depth. With these data one cannot get a sharp enough picture to really explain the details. Understanding sunspots is essential for understanding the 11-year solar cycle, solar flare explosions, and huge coronal mass ejections that affect life and society on Earth. || ",
            "hits": 59
        },
        {
            "id": 3505,
            "url": "https://svs.gsfc.nasa.gov/3505/",
            "result_type": "Visualization",
            "release_date": "2009-10-01T00:00:00-04:00",
            "title": "Solar Cycle 23: Minimum-Maximum-Minimum Synoptic Sequence",
            "description": "This is a sequence of solar synoptic maps covering Solar Cycle 23.The SOHO spacecraft began collecting this data in May of 1996, near the beginning (minimum) of the sunspot cycle. The sequence is projected in cylindrical-equidistant (CED) coordinates suitable for reprojection on spheres for animation or visualization purposes. These images are not suitable for scientific analysis.The original data were collected in FITS format from the SOHO/MDI archive, one image for each Carrington Rotation, which are 27.2753 days long.Solar minimum for Cycle 23 was in May 1996 (Carrington Rotation #1909), solar maximum around March 2000 (Carrington Rotation #1960), with a return to minimum about October 2008 (Carrington Rotation #2075). There are two gaps in the sequence, totalling four rotations, at Carrington rotations #1938, 1939, 1940, 1941, and 1998. These images are missing from the sequence due to SOHO being offline. Gaps in the data coverage for individual maps (occasional day outages or poor coverage near the poles of the Sun) were filled using data accumulated from previous maps.IMPORTANT NOTE: These images are for visualization purposes only. They are not suitable for scientific analysis. || ",
            "hits": 78
        },
        {
            "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": 76
        },
        {
            "id": 3548,
            "url": "https://svs.gsfc.nasa.gov/3548/",
            "result_type": "Visualization",
            "release_date": "2008-09-10T00:00:00-04:00",
            "title": "Comparison: Solar Minimum from SOHO/EIT",
            "description": "This is a short movie of the Sun at the minimum of solar activity. This images are collected in ultraviolet light (a wavelength of 195 Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, few to now sunspots would be visible.At solar minimum, we see few bright active regions. The mottled look is from small 'hot spots' which last less than 48 hours. There are dark regions at the top and bottom of the Sun (corresponding to the north and south solar poles) created by solar magnetic field lines that connect to the interstellar magnetic field. A similar dark region, below the solar equator, is called a coronal hole, where open magnetic field lines enable particles to stream away at high speeds. || ",
            "hits": 36
        },
        {
            "id": 3549,
            "url": "https://svs.gsfc.nasa.gov/3549/",
            "result_type": "Visualization",
            "release_date": "2008-09-10T00:00:00-04:00",
            "title": "Comparison: Solar Maximum from SOHO/EIT",
            "description": "A short movie of the Sun at maximum solar activity as seen in ultraviolet light. These images are collected in ultraviolet light (a wavelength of 195Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, the bright white regions in these images would probably correspond to sunspots.At solar maximum, we see many bright active regions which tend to form in bands in the northern and southern hemispheres. Many of the active regions may eventually launch solar flares or coronal mass ejections (CME). || ",
            "hits": 33
        },
        {
            "id": 3502,
            "url": "https://svs.gsfc.nasa.gov/3502/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/MDI Continuum",
            "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Michelson Doppler Interferometer (MDI) records images at several very narrow wavelength bands in the visible light. These images are often used as proxies for white-light solar images. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are  Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ",
            "hits": 17
        },
        {
            "id": 3503,
            "url": "https://svs.gsfc.nasa.gov/3503/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/MDI Magnetograms",
            "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.The Michelson Doppler Interferometer (MDI) takes images of the Sun at five very narrow wavelength bands and four different polarizations in visible light. For this sequence, the images are processed in a form that reveals the magnetic field strength on the solar photosphere. Other combinations of the images act as white-light images and dopplergrams (which measure the velocity of the solar 'surface').This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are  Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO  For more information, visit the SOHO project page.. || ",
            "hits": 22
        },
        {
            "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": 20
        },
        {
            "id": 20109,
            "url": "https://svs.gsfc.nasa.gov/20109/",
            "result_type": "Animation",
            "release_date": "2007-08-09T00:00:00-04:00",
            "title": "Solar Cycle (Standard Definition)",
            "description": "This animation shows solar activity over a 11 year cycle. For a high definition version of this animation, please go to animation 10185. || ",
            "hits": 11
        },
        {
            "id": 3411,
            "url": "https://svs.gsfc.nasa.gov/3411/",
            "result_type": "Visualization",
            "release_date": "2007-03-22T00:00:00-04:00",
            "title": "Hinode's High-Resolution View of the Sun",
            "description": "A  new sunspot collided with an existing sunspot which built up a  highly sheared magnetic configuration.  This resulted in a solar flare on December 13, 2006. || ",
            "hits": 55
        },
        {
            "id": 3412,
            "url": "https://svs.gsfc.nasa.gov/3412/",
            "result_type": "Visualization",
            "release_date": "2007-03-22T00:00:00-04:00",
            "title": "Hinode's High-resolution view of solar granulation",
            "description": "This zoom-in from a full view of the Hinode Solar Optical Telescope (SOT) (the same as in animation 3411) shows details of solar granulation and how rapidly it changes. || ",
            "hits": 72
        },
        {
            "id": 3336,
            "url": "https://svs.gsfc.nasa.gov/3336/",
            "result_type": "Visualization",
            "release_date": "2006-04-01T00:00:00-05:00",
            "title": "The Visible Sun Revisited",
            "description": "Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar far side (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions before they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts. || ",
            "hits": 37
        },
        {
            "id": 2923,
            "url": "https://svs.gsfc.nasa.gov/2923/",
            "result_type": "Visualization",
            "release_date": "2004-03-08T12:00:00-05:00",
            "title": "SOHO/MDI's 'Window' Through the Sun",
            "description": "Using the mathematical techniques, the SOHO/MDI view of the front side of the Sun can be processed to reveal features on the far side of the Sun. || ",
            "hits": 36
        },
        {
            "id": 20070,
            "url": "https://svs.gsfc.nasa.gov/20070/",
            "result_type": "Animation",
            "release_date": "2003-03-20T12:00:00-05:00",
            "title": "Under the Sunspots",
            "description": "New studies show that the Sun's active regions — areas of intense eruptions — are formed from many small magnetic structures (white loops) that rise from deep within the interior, then pierce the surface to form sunspots (dark areas). These structures appear as giant arches when electrified gas (plasma) passes through their magnetic fields. || ",
            "hits": 31
        },
        {
            "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": 86
        },
        {
            "id": 2656,
            "url": "https://svs.gsfc.nasa.gov/2656/",
            "result_type": "Visualization",
            "release_date": "2003-01-02T12:00:00-05:00",
            "title": "Zoom-out from the Sun",
            "description": "A close-up view of a sunspot group with faculae and pull-out to show the entire Sun. || ",
            "hits": 86
        },
        {
            "id": 2319,
            "url": "https://svs.gsfc.nasa.gov/2319/",
            "result_type": "Visualization",
            "release_date": "2001-12-14T12:00:00-05:00",
            "title": "Temperature Response, Flat Earth Map",
            "description": "Animation of Temperature Response over Flat Earth, 1500 - 1998 C.E. || a002319.00035_print.png (720x480) [346.1 KB] || a002319_thm.png (80x40) [5.2 KB] || a002319_pre.jpg (320x240) [9.0 KB] || a002319_pre_searchweb.jpg (320x180) [71.0 KB] || a002319.webmhd.webm (960x540) [3.5 MB] || a002319.dv (720x480) [61.8 MB] || 640x480_4x3_29.97p (640x480) [32.0 KB] || a002319.mpg (320x240) [2.3 MB] || ",
            "hits": 51
        },
        {
            "id": 2320,
            "url": "https://svs.gsfc.nasa.gov/2320/",
            "result_type": "Visualization",
            "release_date": "2001-12-14T12:00:00-05:00",
            "title": "Solar Radiance Graph",
            "description": "Animation of Temperature Response Graph, 1500 - 1998 C.E. || a002320.00100_print.png (720x480) [94.7 KB] || a002320_pre.jpg (320x240) [3.3 KB] || a002320.webmhd.webm (960x540) [2.2 MB] || a002320.dv (720x480) [84.5 MB] || a002320.mpg (320x240) [1.6 MB] || Temperature Response Graph, 1500 - 1998 C.E. || a002320.jpg (1264x960) [47.7 KB] || a002320_web.jpg (320x243) [3.9 KB] || a002320_thm.png (80x40) [1.1 KB] || a002320_web_searchweb.jpg (320x180) [8.0 KB] || a002320.tif (1264x960) [14.2 KB] || ",
            "hits": 696
        },
        {
            "id": 2321,
            "url": "https://svs.gsfc.nasa.gov/2321/",
            "result_type": "Visualization",
            "release_date": "2001-12-14T12:00:00-05:00",
            "title": "Temperature Response, Global View Over Europe",
            "description": "Animation of Temperature Response over Europe, 1500 - 1998 C.E. || a002321.00050_print.png (720x480) [350.1 KB] || a002321_thm.png (80x40) [2.9 KB] || a002321_pre.jpg (320x240) [6.3 KB] || a002321_pre_searchweb.jpg (180x320) [44.9 KB] || a002321.webmhd.webm (960x540) [1.8 MB] || a002321.dv (720x480) [65.2 MB] || a002321.mpg (320x240) [2.1 MB] || ",
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        {
            "id": 2322,
            "url": "https://svs.gsfc.nasa.gov/2322/",
            "result_type": "Visualization",
            "release_date": "2001-12-14T12:00:00-05:00",
            "title": "Temperature Response, Global View Over North America",
            "description": "Animation of Temperature Response over North America, 1500 - 1998 C.E. || a002322.00005_print.png (720x480) [349.2 KB] || a002322_thm.png (80x40) [2.9 KB] || a002322_pre.jpg (320x240) [6.2 KB] || a002322_pre_searchweb.jpg (320x180) [43.2 KB] || a002322.webmhd.webm (960x540) [1.6 MB] || a002322.dv (720x480) [65.2 MB] || a002322.mpg (320x240) [2.0 MB] || ",
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        {
            "id": 2287,
            "url": "https://svs.gsfc.nasa.gov/2287/",
            "result_type": "Visualization",
            "release_date": "2001-12-10T11:30:00-05:00",
            "title": "The Spinning Sunspot",
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            "url": "https://svs.gsfc.nasa.gov/2304/",
            "result_type": "Visualization",
            "release_date": "2001-12-10T11:30:00-05:00",
            "title": "Under the Rotating Sunspot (Layers 0, 1, 2)",
            "description": "Using the SOHO Michelson Doppler Interferometer (MDI), scientists can use a process called Time-Distance helioseismology to determine temperatures and fluid flows under the surface of the Sun. || ",
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            "url": "https://svs.gsfc.nasa.gov/2314/",
            "result_type": "Visualization",
            "release_date": "2001-12-10T11:30:00-05:00",
            "title": "Temperature and Flows under a Sunspot (Layers 0, 2, 4)",
            "description": "Using the SOHO Michelson Doppler Interferometer (MDI), scientists can use a process called Time-Distance helioseismology to determine temperatures and fluid flows under the surface of the Sun. || ",
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            "url": "https://svs.gsfc.nasa.gov/2232/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Investigates Solar Flows Under Sunspots",
            "description": "SOHO/MDI performs a 'sonogram' of the sun, revealing the subsurface temperature profile around a sunspot.  Red isosurfaces denote regions where the sound speed (and temperature) are higher than average while blue isosurfaces directly under the spot illustrate where the sound speed (and temperature) are lower than average. || ",
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            "url": "https://svs.gsfc.nasa.gov/2243/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Views the Sun - 1998",
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            "id": 2244,
            "url": "https://svs.gsfc.nasa.gov/2244/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Views the Sun - 2001",
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            "url": "https://svs.gsfc.nasa.gov/2268/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Views the Sun - 1998",
            "description": "This version projects the solar image on a flat plane. It runs at a third of the speed of the original version. || SOHO-MDI images the sun from April 30 to June 24, 1998. || a002268.00095_print.png (720x480) [363.2 KB] || a002268_pre.jpg (320x240) [4.3 KB] || a002268.webmhd.webm (960x540) [1.5 MB] || a002268.dv (720x480) [75.5 MB] || a002268.mpg (320x240) [995.0 KB] || ",
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            "id": 2269,
            "url": "https://svs.gsfc.nasa.gov/2269/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Views the Sun - 2001",
            "description": "This version projects the solar image on a flat plane. || A view of the Sun from SOHO-MDI from March thru May 2001. || a002269.00095_print.png (720x480) [379.6 KB] || Sunspots2001_pre.jpg (320x238) [4.2 KB] || a002269.webmhd.webm (960x540) [3.6 MB] || a002269.dv (720x480) [157.8 MB] || Sunspots2001.mpg (352x240) [6.3 MB] || ",
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        {
            "id": 833,
            "url": "https://svs.gsfc.nasa.gov/833/",
            "result_type": "Visualization",
            "release_date": "1999-04-09T12:00:00-04:00",
            "title": "Sun Spot Number Compared with Solar UV from SUSIM (1991-1997)",
            "description": "An animated graph showing the eleven-year sun spot cycle, as shown by measurements of sun spot number. Following this graph, an animation compares sun spot number measurements for the 1990s with direct measurements of the change in solar ultraviolet irradiance from SUSIM. || ",
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        {
            "id": 551,
            "url": "https://svs.gsfc.nasa.gov/551/",
            "result_type": "Visualization",
            "release_date": "1999-01-21T12:00:00-05:00",
            "title": "Delta Sunspot",
            "description": "When a large bundle of magnetic field lines breaks through the Sun's surface, a sunspot can form. Sometimes, a smaller spot will emerge nearby, creating a magnetically complex region where particles are energized and then violently expelled. Supercomputer models show that rearranging magnetic field lines enables this process. || ",
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    ]
}