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    "next": null,
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    "results": [
        {
            "id": 3956,
            "url": "https://svs.gsfc.nasa.gov/3956/",
            "result_type": "Visualization",
            "release_date": "2012-09-20T00:00:00-04:00",
            "title": "Halloween Solar Storms - 2003",
            "description": "This is a 1024x1024 pixel version of solar storms providing a more complete view of the SOHO/LASCO/C3 field-of-view.Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera. || ",
            "hits": 140
        },
        {
            "id": 3755,
            "url": "https://svs.gsfc.nasa.gov/3755/",
            "result_type": "Visualization",
            "release_date": "2010-07-23T00:00:00-04:00",
            "title": "December 2006 Flare from SOHO/EIT and Hinode/XRT",
            "description": "This movie shows data of the December 13, 2006 flare event seen by SOHO/EIT (left) and Hinode XRT (right). The field-of-view of the Hinode images is marked with the yellow border on SOHO/EIT.This movie shows the same event as that in Hinode's High-Resolution View of the Sun. || ",
            "hits": 27
        },
        {
            "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": 78
        },
        {
            "id": 3566,
            "url": "https://svs.gsfc.nasa.gov/3566/",
            "result_type": "Visualization",
            "release_date": "2008-12-18T00:00:00-05:00",
            "title": "Multi-Sun Composition",
            "description": "This movie is a composition of multiple solar datasets synchronized in time. The time frame is late October and early November of 2003, the time of some record-breaking solar activity.The background of the movie shows the view of the wide-angle coronagraphs (blue/white), or LASCO instruments, aboard SOHO. They show streams of electrons outbound from the Sun, part of the solar atmosphere. The central green image is the Sun in ultraviolet light from the EIT instrument. Note that flashes of solar flares in the ultraviolet quickly propagate out from the Sun and are visible in LASCO. These events are coronal mass ejections, or CMEs.Overlaid on the upper left is a better view of the EIT ultraviolet image at a wavelength of 195 angstroms (19.5 nanometers).On the lower left, the orange movie is the EIT ultraviolet movie at 304 angstroms (30.4 nanometers).On the upper right is a solar magnetogram, taken by the MDI instrument. The white regions correspond to positive (north) magnetic flux and the dark regions to negative (south) magnetic flux.The colors for the sequences above are not real. They are chosen by convention since the properties recorded by the cameras are not visible to the human eye.The final image on the lower right is also from MDI. It is a combination of several optical wavelengths and is the best representation from SOHO of the Sun in visible light, as we would see it through ground-based telescopes.The movies that are part of this composition are also available individually on the SVS site: Halloween Solar Storms 2003: SOHO/EIT and SOHO/LASCOHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 195 angstromsHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 304 angstromsHalloween Solar Storms 2003: SOHO/MDI ContinuumHalloween Solar Storms 2003: SOHO/MDI Magnetograms || ",
            "hits": 29
        },
        {
            "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": 46
        },
        {
            "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": 35
        },
        {
            "id": 3535,
            "url": "https://svs.gsfc.nasa.gov/3535/",
            "result_type": "Visualization",
            "release_date": "2008-08-15T00:00:00-04:00",
            "title": "Halloween Storms 2003: SOHO/EIT and TRACE at 195 Angstroms",
            "description": "This visualization compares the full-disk solar view of SOHO/EIT (green, on the left) with the small field of view of the TRACE ultraviolet telescope (gold, on the right). The yellow border of the TRACE imagery is projected on the appropriate location on the green EIT imagery.  Notice that TRACE can track features as they move across the solar disk. The instrument pointing is adjusted on a regular basis, which can produce a considerable amount of jittering in the image. This is a variation on the treatment of the same data as Solar Dynamics Observatory (SDO): Data Collection Comparison.Note that this movie does not play synchronous with the other animations that are part of the SDO Prelaunch package. || ",
            "hits": 24
        },
        {
            "id": 3500,
            "url": "https://svs.gsfc.nasa.gov/3500/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 Angstroms",
            "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 Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 195 angstroms corresponds (19.5 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. 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, 304 A Halloween 2003 Solar Storms: SOHO/MDI Continuum 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": 58
        },
        {
            "id": 3504,
            "url": "https://svs.gsfc.nasa.gov/3504/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO",
            "description": "Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera.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 angstromHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms For more information, visit the SOHO project page.. || ",
            "hits": 51
        },
        {
            "id": 3435,
            "url": "https://svs.gsfc.nasa.gov/3435/",
            "result_type": "Visualization",
            "release_date": "2007-08-14T00:00:00-04:00",
            "title": "Solar Dynamics Observatory (SDO): Data Collection Comparison",
            "description": "Solar Dynamics Observatory (SDO) will dramatically increase our ability to collect data about the Sun. This visualization compares the temporal and spatial resolution of SOHO/EIT with TRACE. SDO will enable TRACE-like image and temporal resolution over the entire solar disk. This movie opens with a full-disk view of the Sun in ultraviolet light (195 angstroms) from SOHO/EIT using the traditional TRACE 'gold' color table. We zoom in on the active region on the western limb where the TRACE instrument is pointing and fade-in an inset of the higher-resolution TRACE data. To emphasize the comparison, the TRACE inset is moved aside (with a solid white border) revealing the matching EIT data view (enclosed in the faint white border). At this point, we step through the time series of data frames. In this movie, much of the TRACE imagery is collected at time intervals between 3 and 40 seconds. On the other hand, a new SOHO/EIT image is taken about every 12 minutes (720 seconds). The SDO Atmospheric Imaging Assembly (AIA) will take full-disk solar images at four times the SOHO/EIT spatial resolution, a whopping 4096x4096, and at least 70 times the temporal resolution, 10 seconds or better per image. This creates a data rate over 1000x higher than SOHO/EIT. It is roughly equivalent to TRACE spatial and temporal resolution, but over the entire solar disk. || ",
            "hits": 80
        },
        {
            "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": 82
        },
        {
            "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": 21
        },
        {
            "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": 49
        },
        {
            "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": 32
        },
        {
            "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": 39
        },
        {
            "id": 2959,
            "url": "https://svs.gsfc.nasa.gov/2959/",
            "result_type": "Visualization",
            "release_date": "2004-07-08T12:00:00-04:00",
            "title": "Halloween Solar Storms from SOHO/EIT, 195 Angstroms",
            "description": "This view from SOHO/EIT in the 195 angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 and 2961. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ",
            "hits": 27
        },
        {
            "id": 2961,
            "url": "https://svs.gsfc.nasa.gov/2961/",
            "result_type": "Visualization",
            "release_date": "2004-07-08T12:00:00-04:00",
            "title": "Halloween Solar Storms from SOHO/EIT and SOHO/LASCO",
            "description": "This movie is a combination of SOHO/EIT at 195 angstroms as well as the LASCO/C2 and C3 cameras. At this scale we can see the flashes from solar flares in SOHO/EIT (green) and the subsequent coronal mass ejections in SOHO/LASCO/C2 (red) and SOHO/LASCO/C3 (blue). This movie is synchronized to play with animation IDs 2960 and 2959. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ",
            "hits": 41
        },
        {
            "id": 2936,
            "url": "https://svs.gsfc.nasa.gov/2936/",
            "result_type": "Visualization",
            "release_date": "2004-05-23T12:00:00-04:00",
            "title": "The fastest CME of Cycle 23 overtakes another fast CME",
            "description": "On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft. || ",
            "hits": 59
        },
        {
            "id": 2917,
            "url": "https://svs.gsfc.nasa.gov/2917/",
            "result_type": "Visualization",
            "release_date": "2004-02-20T12:00:00-05:00",
            "title": "SORCE Monitors Solar Variability during Record Solar Flares",
            "description": "The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. || ",
            "hits": 30
        },
        {
            "id": 2918,
            "url": "https://svs.gsfc.nasa.gov/2918/",
            "result_type": "Visualization",
            "release_date": "2004-02-20T12:00:00-05:00",
            "title": "SORCE Monitors Solar Variability during Record Solar Flares - Video version",
            "description": "The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video. || ",
            "hits": 66
        },
        {
            "id": 2509,
            "url": "https://svs.gsfc.nasa.gov/2509/",
            "result_type": "Visualization",
            "release_date": "2003-01-31T12:00:00-05:00",
            "title": "A Multi-Mission View of the AR9906 Solar Flare with Instrument Labels",
            "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from six hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, the instrument names appear in a color roughly matching the color used for the data, and black corresponds to no (current) instrument coverage. || ",
            "hits": 11
        },
        {
            "id": 2511,
            "url": "https://svs.gsfc.nasa.gov/2511/",
            "result_type": "Visualization",
            "release_date": "2003-01-31T12:00:00-05:00",
            "title": "A Multi-Mission View of the AR9906 Solar Flare without Instrument Labels",
            "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ",
            "hits": 9
        },
        {
            "id": 2553,
            "url": "https://svs.gsfc.nasa.gov/2553/",
            "result_type": "Visualization",
            "release_date": "2003-01-31T12:00:00-05:00",
            "title": "A Multi-Mission View of the AR9906 Solar Flare with Alternate Instrument Labels",
            "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ",
            "hits": 32
        },
        {
            "id": 2495,
            "url": "https://svs.gsfc.nasa.gov/2495/",
            "result_type": "Visualization",
            "release_date": "2002-07-25T12:00:00-04:00",
            "title": "SOHO/EIT views solar 'Grand Slam'",
            "description": "A full view of the sun at 195 angstroms from SOHO/EIT. The time covers July 15-23, 2002. Four X-class flares erupted: an X3.0 on July 15, an X1.8 on July 18, a X3.3 on July 20 and an X4.0 on July 23. || ",
            "hits": 8
        },
        {
            "id": 2496,
            "url": "https://svs.gsfc.nasa.gov/2496/",
            "result_type": "Visualization",
            "release_date": "2002-07-25T12:00:00-04:00",
            "title": "SOHO/EIT Views Solar 'Grand Slam' with Zoom",
            "description": "A view of the sun at 195 angstroms from SOHO/EIT. The time covers July 15-23, 2002. Four X-class flares erupted: an X3.0 on July 15, an X1.8 on July 18, a X3.3 on July 20 and an X4.0 on July 23. The version zooms in slightly to the flare region. || ",
            "hits": 16
        },
        {
            "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": 14
        },
        {
            "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": 14
        },
        {
            "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": 12
        },
        {
            "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": 2402,
            "url": "https://svs.gsfc.nasa.gov/2402/",
            "result_type": "Visualization",
            "release_date": "2002-03-20T12:00:00-05:00",
            "title": "First Flare movie for the RHESSI Instrument (Speed 105x Normal)",
            "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at the maximum speed of one frame corresponding to 3.5 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ",
            "hits": 14
        },
        {
            "id": 2403,
            "url": "https://svs.gsfc.nasa.gov/2403/",
            "result_type": "Visualization",
            "release_date": "2002-03-20T12:00:00-05:00",
            "title": "First Flare Movie for the RHESSI Instrument (Speed 52x Normal)",
            "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at a speed of two video frames corresponding to 3.5 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ",
            "hits": 13
        },
        {
            "id": 2404,
            "url": "https://svs.gsfc.nasa.gov/2404/",
            "result_type": "Visualization",
            "release_date": "2002-03-20T12:00:00-05:00",
            "title": "First Flare Movie for the RHESSI Instrument (Speed 26x Normal)",
            "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at a speed of four video frames corresponding to 3.75 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ",
            "hits": 17
        }
    ]
}