{
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    "results": [
        {
            "id": 14907,
            "url": "https://svs.gsfc.nasa.gov/14907/",
            "result_type": "Produced Video",
            "release_date": "2025-09-30T14:00:00-04:00",
            "title": "What is space weather?",
            "description": "Though it is almost 100 million miles away from Earth, the Sun influences our daily lives in ways you may not realize.A farmer stops their planting operations due to poor GPS signal for their autonomous tractor. A power grid manager changes the configuration of their network to ensure a blackout doesn’t occur due to voltage instability. A pilot switches to back-up communication equipment due to loss of high-frequency radio. A commercial internet company providing service to the military must change the orbit of their spacecraft to avoid a collision due to increased atmospheric drag.These are a few examples of the ways the Sun influences our everyday lives. This is what we define as space weather – the conditions of the space environment driven by the Sun and its impacts on objects in the solar system. || ",
            "hits": 234
        },
        {
            "id": 5280,
            "url": "https://svs.gsfc.nasa.gov/5280/",
            "result_type": "Visualization",
            "release_date": "2024-07-02T00:00:00-04:00",
            "title": "An X4.5 flare from Active Region 13663 - May 6, 2024",
            "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Lots of coronal loop motion precedes the launch of an X4.5 flare from Active Region 13663 on May 6, 2024 (upper right quadrant).  More details of this event can be found at the Space Weather Database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ",
            "hits": 16
        },
        {
            "id": 5165,
            "url": "https://svs.gsfc.nasa.gov/5165/",
            "result_type": "Visualization",
            "release_date": "2024-01-05T00:00:00-05:00",
            "title": "STEREO - The Second Time Around...",
            "description": "In mid-August 2023, the still-operational STEREO-A (STEREO-B went offline in October 2014) passed Earth for the first time since its launch 17 years ago. See also STEREO-A Returns by Earth.While STEREO-B is no longer available, it is possible to construct stereo imagery of the Sun using STEREO-A with Solar Dynamics Observatory (SDO).  Here we present a series of images for corresponding filters between the two missions which can be used for stereo viewing.Color (SDO color table) Left/Right Image PairsIn this section, we present frame-synchronized left eye (STEREO-A) and right eye (SDO) for the specified ultraviolet filter.  They are provided as separate movie and frame-sets to maximize flexibility for the target viewing technology.  Time stamps are provided as separate image files for compositing if desired.   If you match frame numbers for the image sets for a specific filter, you will have images closest in time for apropriate left/right eye pairing.171 Angstrom filter || ",
            "hits": 70
        },
        {
            "id": 5201,
            "url": "https://svs.gsfc.nasa.gov/5201/",
            "result_type": "Visualization",
            "release_date": "2023-12-13T00:00:00-05:00",
            "title": "M 9.8 flare at Active Region 13500 - November 28, 2023",
            "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13500 near the center of the solar disk erupts with a class M9.8 flare.  A nice loop arcade forms, apparently as part of the eruption.  For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ",
            "hits": 17
        },
        {
            "id": 5159,
            "url": "https://svs.gsfc.nasa.gov/5159/",
            "result_type": "Visualization",
            "release_date": "2023-09-20T00:00:00-04:00",
            "title": "M 6.0 flare at Active Region 13413 - September 3, 2023",
            "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13413 on the limb of the Sun erupts with mid-range flare exceeding M5 intensity.  A nice loop arcade forms, apparently as part of the eruption.  For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ",
            "hits": 20
        },
        {
            "id": 4966,
            "url": "https://svs.gsfc.nasa.gov/4966/",
            "result_type": "Visualization",
            "release_date": "2022-08-19T00:00:00-04:00",
            "title": "AR 12938 - Slow Building Active Region on Left Limb",
            "description": "The slow build-up of a solar active region, as seen in AIA 171 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF). || AR12938_AIA171_stamped.001680_print.jpg (1024x1024) [235.2 KB] || AR12938_AIA171_stamped.001680_searchweb.png (320x180) [89.7 KB] || AR12938_AIA171_stamped.001680_thm.png (80x40) [6.7 KB] || AR12938_AIA171_PSF_2048p30.mp4 (2048x2048) [261.0 MB] || AR12938_AIA171_PSF_stamped_2048p30.mp4 (2048x2048) [262.2 MB] || AR12938_AIA171_stamped_1024p30.mp4 (1024x1024) [33.1 MB] || AR12938_AIA171_stamped_1024p30.webm (1024x1024) [7.1 MB] || AIA171-Frames.PSF (4096x4096) [128.0 KB] || AIA171-Frames.PSF.stamped (4096x4096) [128.0 KB] || AIA171-Time.PSF (4096x4096) [128.0 KB] || AR12938_AIA171_PSF_4096p30_h265.mp4 (4096x4096) [813.9 MB] || AR12938_AIA171_PSF_stamped_4096p30_h265.mp4 (4096x4096) [814.7 MB] || ",
            "hits": 19
        },
        {
            "id": 14159,
            "url": "https://svs.gsfc.nasa.gov/14159/",
            "result_type": "Produced Video",
            "release_date": "2022-05-06T12:00:00-04:00",
            "title": "Active Sun in Early May, 2022",
            "description": "NASA’s Solar Dynamics Observatory captured this image of an X1.1 solar flare – as seen in the bright flash in the upper right portion of the image – on May 3, 2022 at 13:25 UTC. The image is a wavelength of extreme ultraviolet light – 131 angstrom –  that highlights the extremely hot material in flares and which is colorized teal.Credit: NASA/SDO || 20220503_FlareX11_131A.00146_print.jpg (1024x1024) [302.4 KB] || 20220503_FlareX11_131A.00146_searchweb.png (320x180) [60.4 KB] || 20220503_FlareX11_131A.00146_thm.png (80x40) [5.1 KB] || 20220503_FlareX11_131A.00146.tiff (4096x4096) [64.0 MB] || ",
            "hits": 30
        },
        {
            "id": 13982,
            "url": "https://svs.gsfc.nasa.gov/13982/",
            "result_type": "Produced Video",
            "release_date": "2021-10-28T14:00:00-04:00",
            "title": "Active October Sun Emits X-class Flare",
            "description": "Brighter than a shimmering ghost, faster than the flick of a black cat’s tail, the Sun cast a spell in our direction, just in time for Halloween. This imagery captured by NASA’s Solar Dynamics Observatory covers a busy few days of activity between Oct. 25-28 that ended with a significant solar flare. From late afternoon Oct. 25 through mid-morning Oct. 26, an active region on the left limb of the Sun flickered with a series of small flares and petal-like eruptions of solar material. Meanwhile, the Sun was sporting more active regions at its lower center, directly facing Earth. On Oct. 28, the biggest of these released a significant flare, which peaked at 11:35 a.m. EDT. Credit: NASA/GSFC/SDOMusic: \"Immersion\" from Above and Below.  Written and produced by Lars LeonhardWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || ActiveOctober_Still.jpg (1920x1080) [956.2 KB] || 13982_ActiveOctober_ProRes_1920x1080_2997.mov (1920x1080) [2.4 GB] || 13982_ActiveOctober_1080_Best.mp4 (1920x1080) [436.2 MB] || 13982_ActiveOctober_1080.mp4 (1920x1080) [188.1 MB] || 13982_ActiveOctober_1080_Best.webm (1920x1080) [19.7 MB] || 13982_ActiveOctober_SRT_Captions.en_US.srt [574 bytes] || 13982_ActiveOctober_SRT_Captions.en_US.vtt [587 bytes] || ",
            "hits": 79
        },
        {
            "id": 4766,
            "url": "https://svs.gsfc.nasa.gov/4766/",
            "result_type": "Visualization",
            "release_date": "2020-09-21T11:00:00-04:00",
            "title": "IRIS views Nano-Flares on the Sun",
            "description": "Opening full-disk solar view from AIA 304 angstroms, zooming in and fading in IRIS SJI at 1400 angstroms. || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i.00663_print.jpg (1024x576) [139.8 KB] || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i.00663_searchweb.png (320x180) [67.9 KB] || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i.00663_thm.png (80x40) [5.0 KB] || SDO304-IRIS1400-nanoflare2014-zoomHD (1920x1080) [0 Item(s)] || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i_p30.mp4 (1920x1080) [60.5 MB] || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i_p30.webm (1920x1080) [3.0 MB] || SDO304-IRIS1400-nanoflare2014-zoomHD (3840x2160) [0 Item(s)] || SDO304-IRIS1400-nanoflare2014-zoom_stand.UHD2160_p30.mp4 (3840x2160) [203.9 MB] || SDO304-IRIS1400-nanoflare2014-zoom_stand.HD1080i_p30.mp4.hwshow [218 bytes] || ",
            "hits": 24
        },
        {
            "id": 4323,
            "url": "https://svs.gsfc.nasa.gov/4323/",
            "result_type": "Visualization",
            "release_date": "2016-02-11T00:00:00-05:00",
            "title": "Summer Sun from SDO: Eruption and Coronal Loops on the Solar Limb",
            "description": "HD1080 movie of the Sun in the AIA 304 angstrom filter.  Note the coronal loop structures on the lower right limb. || June2015LimbLoops_304A_stand.HD1080i.00256_print.jpg (1024x576) [68.0 KB] || June2015LimbLoops_304A_1080p.webm (1920x1080) [5.1 MB] || June2015LimbLoops_304AHD (1920x1080) [128.0 KB] || June2015LimbLoops_304A_1080p.mp4 (1920x1080) [34.7 MB] || June2015LimbLoops_304A.HD1080.mov (1920x1080) [108.5 MB] || June2015LimbLoops_304A_1080p.mp4.hwshow [228 bytes] || ",
            "hits": 51
        },
        {
            "id": 4391,
            "url": "https://svs.gsfc.nasa.gov/4391/",
            "result_type": "Visualization",
            "release_date": "2016-01-29T10:00:00-05:00",
            "title": "The Dynamic Solar Magnetic Field",
            "description": "A visualization of the slow changes of the solar magnetic field over the course of four years. || PFSSbasicView_inertial.HD1080i.0400_print.jpg (1024x576) [168.7 KB] || PFSSbasicView_inertial.HD1080i.0400_searchweb.png (180x320) [78.9 KB] || PFSSbasicView_inertial.HD1080i.0400_thm.png (80x40) [5.8 KB] || PFSSbasicView_inertial_1080p30.webm (1920x1080) [18.1 MB] || PFSSbasicView (1920x1080) [128.0 KB] || PFSSbasicView_inertial_1080p30.mp4 (1920x1080) [326.6 MB] || PFSSbasicView_inertial_1080p10.mp4 (1920x1080) [470.2 MB] || PFSSbasicView_HD1080p10.mov (1920x1080) [804.4 MB] || PFSSbasicView_inertial_1080p30.mp4.hwshow [232 bytes] || ",
            "hits": 144
        },
        {
            "id": 12104,
            "url": "https://svs.gsfc.nasa.gov/12104/",
            "result_type": "Produced Video",
            "release_date": "2016-01-29T10:00:00-05:00",
            "title": "The Dynamic Solar Magnetic Field - Narrated",
            "description": "Holly Gilbert, NASA GSFC solar scientist, explains a model of magnetic fields on the sun. || thumb.jpg (1280x720) [156.8 KB] || thumb_searchweb.png (320x180) [124.7 KB] || thumb_thm.png (80x40) [20.5 KB] || 12104_b-roll.mov (1280x720) [2.0 GB] || 12104_original.mov (1920x1080) [3.8 GB] || 12104_youtube_hq.mov (1920x1080) [1.7 GB] || 12104_appletv.m4v (1280x720) [63.5 MB] || 12104_b-roll.webm (1280x720) [24.5 MB] || 12104_lowres.mp4 (480x272) [19.2 MB] || ",
            "hits": 89
        },
        {
            "id": 4309,
            "url": "https://svs.gsfc.nasa.gov/4309/",
            "result_type": "Visualization",
            "release_date": "2015-05-28T00:00:00-04:00",
            "title": "Blast from the Past: A Flare from January 2012",
            "description": "A 1080 HD Full-Disk movie of the flare event. || Jan2012Flare_171A_stand.HD1080i.01500_print.jpg (1024x576) [69.7 KB] || Jan2012Flare_171A_stand.HD1080i.01500_searchweb.png (320x180) [47.1 KB] || Jan2012Flare_171A_stand.HD1080i.01500_thm.png (80x40) [4.3 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Jan2012Flare_171A_stand_1080p30.mp4 (1920x1080) [33.7 MB] || Jan2012Flare_171A_stand_1080p30.mov (1920x1080) [86.4 MB] || Jan2012Flare_171A_stand_1080p30.webm (1920x1080) [9.4 MB] || Jan2012Flare_171A_stand_1080p30.mp4.hwshow [197 bytes] || ",
            "hits": 29
        },
        {
            "id": 4089,
            "url": "https://svs.gsfc.nasa.gov/4089/",
            "result_type": "Visualization",
            "release_date": "2014-02-11T10:00:00-05:00",
            "title": "June 2013's 'Busy Sun'",
            "description": "June of 2013, near the maximum of solar cycle 24, while not extremely active from a solar flare perspective, presented a range of diverse phenomena. We have a couple of solar 'tornadoes' (the twisted protrusions off the limb of the Sun in upper and lower left quadrants), which we eventually see erupt material into space. There are also a number of coronal loops in active regions which are incredibly stable but still exhibit much fine detail. || ",
            "hits": 38
        },
        {
            "id": 11385,
            "url": "https://svs.gsfc.nasa.gov/11385/",
            "result_type": "Produced Video",
            "release_date": "2013-12-17T10:00:00-05:00",
            "title": "Jewel Box Sun",
            "description": "Telescopes help distant objects appear bigger, but this is only one of their advantages. Telescopes can also collect light in ranges that our eyes alone cannot see, providing scientists ways of observing a whole host of material and processes that would otherwise be inaccessible. A new NASA movie of the sun based on data from NASA's Solar Dynamics Observatory, or SDO, shows the wide range of wavelengths – invisible to the naked eye – that the telescope can view. SDO converts the wavelengths into an image humans can see, and the light is colorized into a rainbow of colors. As the colors sweep around the sun in the movie, viewers should note how different the same area of the sun appears. This happens because each wavelength of light represents solar material at specific temperatures. Different wavelengths convey information about different components of the sun's surface and atmosphere, so scientists use them to paint a full picture of our constantly changing and varying star.Yellow light of 5800 angstroms, for example, generally emanates from material of about 10,000 degrees F (5700 degrees C), which represents the surface of the sun. Extreme ultraviolet light of 94 angstroms, which is typically colorized in green in SDO images, comes from atoms that are about 11 million degrees F (6,300,000 degrees C) and is a good wavelength for looking at solar flares, which can reach such high temperatures. By examining pictures of the sun in a variety of wavelengths – as is done not only by SDO, but also by NASA's Interface Region Imaging Spectrograph, NASA's Solar Terrestrial Relations Observatory and the European Space Agency/NASA Solar and Heliospheric Observatory — scientists can track how particles and heat move through the sun's atmosphere. || ",
            "hits": 102
        },
        {
            "id": 10817,
            "url": "https://svs.gsfc.nasa.gov/10817/",
            "result_type": "Produced Video",
            "release_date": "2011-09-07T12:00:00-04:00",
            "title": "SDO EVE Late Phase Flares",
            "description": "Scientists have been seeing just the tip of the iceberg when monitoring flares with X-rays. With the complete extreme ultraviolet (EUV) coverage by the SDO EUV Variability Experiment (EVE), they have observed enhanced EUV radiation that appears not only during the X-ray flare, but also a second time delayed by many minutes after the X-ray flare peak. These delayed, second peaks are referred to as the EUV Late Phase contribution to flares.The solar EUV radiation creates our Earth's ionosphere (plasma in our atmosphere), so solar flares disturb our ionosphere and consequently our communication and navigation technologies, such as Global Positioning System (GPS), that transmit through the ionosphere. For over 30 years, scientists have relied on the GOES X-ray monitor to tell them when to expect disturbances to our ionosphere. With these new SDO EVE results, they now recognize that additional ionospheric disturbances from these later EUV enhancements are also a concern. || ",
            "hits": 73
        },
        {
            "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": 32
        },
        {
            "id": 40059,
            "url": "https://svs.gsfc.nasa.gov/gallery/solar-phenomena/",
            "result_type": "Gallery",
            "release_date": "2010-03-04T00:00:00-05:00",
            "title": "Solar Phenomena",
            "description": "No description available.",
            "hits": 13
        },
        {
            "id": 3346,
            "url": "https://svs.gsfc.nasa.gov/3346/",
            "result_type": "Visualization",
            "release_date": "2006-03-30T00:00:00-05:00",
            "title": "Grand Tour of the Coronal Loops Model",
            "description": "This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT standard color table. || ",
            "hits": 68
        },
        {
            "id": 3286,
            "url": "https://svs.gsfc.nasa.gov/3286/",
            "result_type": "Visualization",
            "release_date": "2005-10-27T00:00:00-04:00",
            "title": "Flight through the Coronal Loops",
            "description": "Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT 'standard color table'. || ",
            "hits": 34
        },
        {
            "id": 3287,
            "url": "https://svs.gsfc.nasa.gov/3287/",
            "result_type": "Visualization",
            "release_date": "2005-10-27T00:00:00-04:00",
            "title": "Rotating Tour of Solar Coronal Loops",
            "description": "A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. || ",
            "hits": 58
        },
        {
            "id": 3159,
            "url": "https://svs.gsfc.nasa.gov/3159/",
            "result_type": "Visualization",
            "release_date": "2005-05-24T12:00:00-04:00",
            "title": "SOHO/LASCO View of January 2005 Solar Events",
            "description": "The January 20 flare began just before 2 a.m. ET. A storm of energetic protons impacted Earth just 15 minutes later. These views of the flare are from the Solar and Heliospheric Observatory (SOHO). The proton storm near Earth causes `snow' in the images, obscuring the Sun as radiation swamps the cameras. The structure at the 1:30 position in the SOHO/LASCO/C3 data is the occulting disk pylon. || ",
            "hits": 21
        },
        {
            "id": 3160,
            "url": "https://svs.gsfc.nasa.gov/3160/",
            "result_type": "Visualization",
            "release_date": "2005-05-24T12:00:00-04:00",
            "title": "January 2005 Solar Flares from SOHO/EIT",
            "description": "SOHO/EIT's view of the Sun in late January 2005. || fast_eit.0000.jpg (720x480) [44.6 KB] || fast_eit_320x240_pre.jpg (320x240) [8.1 KB] || fast_eit_NTSC.webmhd.webm (960x540) [4.1 MB] || fast_eit_640x480.mpg (640x480) [15.0 MB] || fast_eit_NTSC.m2v (720x480) [24.0 MB] || 720x480_4x3_30 (720x480) [32.0 KB] || a003160_fast_eit_NTSC.mp4 (640x480) [4.8 MB] || fast_eit_320x240.mpg (320x240) [3.9 MB] || ",
            "hits": 21
        },
        {
            "id": 3161,
            "url": "https://svs.gsfc.nasa.gov/3161/",
            "result_type": "Visualization",
            "release_date": "2005-05-24T12:00:00-04:00",
            "title": "TRACE Ultraviolet View of January 20, 2005 Solar Flare",
            "description": "AR 10720 in the TRACE 1600 angstrom band. || fast_trace.0000.jpg (720x480) [59.4 KB] || fast_trace_320x240_pre.jpg (320x240) [9.6 KB] || fast_trace_NTSC.webmhd.webm (960x540) [7.1 MB] || fast_trace_640x480.mpg (640x480) [12.2 MB] || fast_trace_NTSC.m2v (720x480) [19.5 MB] || 720x480_4x3_30 (720x480) [32.0 KB] || a003161_fast_trace_NTSC.mp4 (640x480) [3.9 MB] || fast_trace_320x240.mpg (320x240) [3.1 MB] || ",
            "hits": 24
        },
        {
            "id": 2750,
            "url": "https://svs.gsfc.nasa.gov/2750/",
            "result_type": "Visualization",
            "release_date": "2003-09-02T12:00:00-04:00",
            "title": "RHESSI Observes 2.2 MeV Line Emission from a Solar Flare",
            "description": "The solar flare at Active Region 10039 on July 23, 2002 exhibits many exceptional high-energy phenomena including the 2.223 MeV neutron capture line and the 511 keV electron-positron (antimatter) annihilation line. In the animation, the RHESSI low-energy channels (12-25 keV) are represented in red and appears predominantly in coronal loops. The high-energy flux appears as blue at the footpoints of the coronal loops. Violet is used to indicate the location and relative intensity of the 2.2MeV emission. || ",
            "hits": 20
        },
        {
            "id": 2717,
            "url": "https://svs.gsfc.nasa.gov/2717/",
            "result_type": "Visualization",
            "release_date": "2003-04-11T12:00:00-04:00",
            "title": "Closeup of Solar 'Tadpoles' with time tags",
            "description": "Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE.  One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare.  This version of the visualization displays the instrument clock time tags. || ",
            "hits": 10
        },
        {
            "id": 2718,
            "url": "https://svs.gsfc.nasa.gov/2718/",
            "result_type": "Visualization",
            "release_date": "2003-04-11T12:00:00-04:00",
            "title": "Closeup of Solar 'Tadpoles' without time tags",
            "description": "Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE.  One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare.  This version of the visualization does not display the instrument clock time tags. || ",
            "hits": 5
        },
        {
            "id": 2464,
            "url": "https://svs.gsfc.nasa.gov/2464/",
            "result_type": "Visualization",
            "release_date": "2002-06-10T12:00:00-04:00",
            "title": "Another View of AR9906 from TRACE",
            "description": "Another view of the flare over AR9906 on April 21, 2002.  This version represents the full resolution of the TRACE data.  This visualization represents eight hours of observing time. || ",
            "hits": 6
        },
        {
            "id": 2458,
            "url": "https://svs.gsfc.nasa.gov/2458/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - Time Tagged",
            "description": "Close-up view of the solar active region AR9906 on April 21, 2002 with TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ",
            "hits": 11
        },
        {
            "id": 2459,
            "url": "https://svs.gsfc.nasa.gov/2459/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - No time tags",
            "description": "Close-up view of the solar active region AR9906 on April 21, 2002 with TRACE data and RHESSI. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ",
            "hits": 7
        },
        {
            "id": 2460,
            "url": "https://svs.gsfc.nasa.gov/2460/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - zoom with times",
            "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || Movie of RHESSI and TRACE data. || a002460.00100_print.png (720x480) [447.6 KB] || ar9906-zoom-dates_pre.jpg (320x240) [6.9 KB] || a002460.webmhd.webm (960x540) [6.9 MB] || ar9906-zoom-dates.mpg (640x480) [15.0 MB] || a002460.dv (720x480) [118.8 MB] || ",
            "hits": 12
        },
        {
            "id": 2461,
            "url": "https://svs.gsfc.nasa.gov/2461/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - zoom without times",
            "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ",
            "hits": 9
        },
        {
            "id": 2462,
            "url": "https://svs.gsfc.nasa.gov/2462/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - rotate view with times",
            "description": "Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO/EIT,TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ",
            "hits": 16
        },
        {
            "id": 2463,
            "url": "https://svs.gsfc.nasa.gov/2463/",
            "result_type": "Visualization",
            "release_date": "2002-06-05T12:00:00-04:00",
            "title": "RHESSI Observes the Flare over AR9906 - Rotate View Without Times",
            "description": "Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ",
            "hits": 12
        },
        {
            "id": 2446,
            "url": "https://svs.gsfc.nasa.gov/2446/",
            "result_type": "Visualization",
            "release_date": "2002-05-29T12:00:00-04:00",
            "title": "TRACE Observes the X-ray Flare Over AR9906",
            "description": "The TRACE spacecraft observes an X-ray flare over solar active region AR9906, April 21, 2002. || Movie of the flaring of active region AR9906 || a002446.00070_print.png (720x480) [447.5 KB] || xflare-ar9906_pre.jpg (320x240) [5.3 KB] || a002446.webmhd.webm (960x540) [2.1 MB] || a002446.dv (720x480) [44.6 MB] || xflare-ar9906.mpg (320x240) [1.7 MB] || ",
            "hits": 14
        },
        {
            "id": 1168,
            "url": "https://svs.gsfc.nasa.gov/1168/",
            "result_type": "Visualization",
            "release_date": "2000-06-13T12:00:00-04:00",
            "title": "'Bastille Day' Flare Animation",
            "description": "Fly-in of TRACE full sun image to the flare location.  Fade to a model of the field lines with a magnetogram of the solar surface.  Pull back out to display a movie of  flare images.  This version uses lens flares to illustrate matter motion along the field lines. || ",
            "hits": 14
        },
        {
            "id": 1169,
            "url": "https://svs.gsfc.nasa.gov/1169/",
            "result_type": "Visualization",
            "release_date": "2000-06-13T12:00:00-04:00",
            "title": "Bastille Day Flare Without Matter Motion",
            "description": "Fly-in of TRACE full sun image to the flare location. Fade to a model of the field lines with a magnetogram of the solar surface. Pull back out to display a movie of flare images. This version does not show the matter motion along the field lines. || ",
            "hits": 12
        },
        {
            "id": 689,
            "url": "https://svs.gsfc.nasa.gov/689/",
            "result_type": "Visualization",
            "release_date": "1999-07-14T12:00:00-04:00",
            "title": "TRACE: Viewing a Coronal Loop with a Diagram of the Earth for Scale.",
            "description": "Zooming into the sun to show an animation of the Bastille Day solar flare from TRACE imagery || a000689.00010_print.png (720x480) [443.9 KB] || TRACE_pre.jpg (320x240) [6.2 KB] || a000689_pre.jpg (320x242) [6.3 KB] || a000689.webmhd.webm (960x540) [3.6 MB] || a000689.dv (720x480) [54.9 MB] || a000689.mp4 (640x480) [4.6 MB] || TRACE.mov (320x240) [934.9 KB] || a000689.mpg (352x240) [3.0 MB] || ",
            "hits": 49
        },
        {
            "id": 690,
            "url": "https://svs.gsfc.nasa.gov/690/",
            "result_type": "Visualization",
            "release_date": "1999-07-14T12:00:00-04:00",
            "title": "TRACE: Viewing a Coronal Loop",
            "description": "Zooming into the sun to show an animation of the Bastille Day solar flare from TRACE imagery || a000690.00010_print.png (720x480) [439.2 KB] || a000690_pre.jpg (320x242) [6.3 KB] || a000690.webmhd.webm (960x540) [3.6 MB] || a000690.dv (720x480) [51.5 MB] || a000690.mp4 (640x480) [4.5 MB] || a000690.mpg (352x240) [3.1 MB] || ",
            "hits": 51
        },
        {
            "id": 691,
            "url": "https://svs.gsfc.nasa.gov/691/",
            "result_type": "Visualization",
            "release_date": "1999-07-14T12:00:00-04:00",
            "title": "TRACE: A Coronal Loop with a Co-temporal Yohkoh Soft X-ray Image Overlaid",
            "description": "An image of a coronal loop from TRACE, with a co-temporal soft x-ray image from YOKOH overlaid || a000691.00010_print.png (720x480) [457.8 KB] || a000691_thm.png (80x40) [6.3 KB] || a000691_pre.jpg (320x238) [7.7 KB] || a000691_pre_searchweb.jpg (320x180) [56.6 KB] || a000691.webmhd.webm (960x540) [434.6 KB] || a000691.dv (720x480) [24.0 MB] || a000691.mp4 (640x480) [2.0 MB] || a000691.mpg (352x240) [1.5 MB] || ",
            "hits": 37
        }
    ]
}