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    "results": [
        {
            "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": 109
        },
        {
            "id": 4128,
            "url": "https://svs.gsfc.nasa.gov/4128/",
            "result_type": "Visualization",
            "release_date": "2013-12-24T00:00:00-05:00",
            "title": "Solar Dynamics Observatory - Argo view - Slices of SDO",
            "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections. This visualization is a variation of the original Solar Dynamics Observatory - Argo view. In this case, the different wavelength filters are presented in three sets around the Sun at full 4Kx4K resolution. This enables monitoring of changes in time over all wavelengths at any location around the limb of the Sun. The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.if we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.in far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ",
            "hits": 69
        },
        {
            "id": 4117,
            "url": "https://svs.gsfc.nasa.gov/4117/",
            "result_type": "Visualization",
            "release_date": "2013-12-17T10:00:00-05:00",
            "title": "Solar Dynamics Observatory - Argo view",
            "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections.The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.Small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.If we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.In far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ",
            "hits": 88
        },
        {
            "id": 3986,
            "url": "https://svs.gsfc.nasa.gov/3986/",
            "result_type": "Visualization",
            "release_date": "2012-11-20T09:00:00-05:00",
            "title": "The Active Sun from SDO: 1700 Ångstroms",
            "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.This movie is generated for a wavelength of 1700 Ånstroms (170.0 nanometers) which is in the ultraviolet band showing the lower level of the Sun's atmosphere, called the chromosphere.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ",
            "hits": 68
        },
        {
            "id": 4008,
            "url": "https://svs.gsfc.nasa.gov/4008/",
            "result_type": "Visualization",
            "release_date": "2012-11-20T09:00:00-05:00",
            "title": "SDO Jewelbox: The Many Eyes of SDO",
            "description": "5x3 Layout view. This version has the imagery organized in order of increasing wavelength, from upper left to lower right for AIA. The HMI products occupy the bottom row. || SDOJewelbox_5x3.0100.jpg (2400x810) [317.7 KB] || SDOJewelbox_5x3.0100_web.png (320x108) [28.9 KB] || SDOJewelbox_5x3.0100_thm.png (80x40) [3.7 KB] || SDOJewelbox_5x3.0100_searchweb.png (320x180) [29.2 KB] || SDOJewelbox_5x3.webmhd.webm (960x540) [3.3 MB] || SDOJewelbox_5x3.mov (2400x810) [91.5 MB] || SDOJewelbox_5x3.mp4 (2400x810) [91.5 MB] || 2400x810_80x27_30p (2400x810) [0 Item(s)] || ",
            "hits": 92
        },
        {
            "id": 3841,
            "url": "https://svs.gsfc.nasa.gov/3841/",
            "result_type": "Visualization",
            "release_date": "2011-07-01T10:00:00-04:00",
            "title": "Incredible Solar Flare, Prominence Eruption and CME Event (1700 angstroms)",
            "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). At this wavelength, very little of the ejected material is visible. However, it is possible to see locations where some of the material is falling back and striking the solar surface.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3840 (211 Ångstroms) and 3838 (304 Ångstroms). || ",
            "hits": 36
        },
        {
            "id": 10801,
            "url": "https://svs.gsfc.nasa.gov/10801/",
            "result_type": "Produced Video",
            "release_date": "2011-06-30T09:00:00-04:00",
            "title": "Massive Solar Eruption Close-up",
            "description": "On June 7, 2011 the Sun unleashed an M-2 (medium-sized) solar flare with a spectacular coronal mass ejection (CME). The large cloud of particles mushroomed up and fell back down looking as if it covered an area almost half the solar surface.SDO observed the flare's peak at 1:41 AM ET. SDO recorded these images in extreme ultraviolet light that show a very large eruption of cool gas. It is somewhat unique because at many places in the eruption there seems to be even cooler material — at temperatures less than 80,000 K.This video uses the full-resolution 4096 x 4096 pixel images at a one minute time cadence to provide the highest quality, finest detail version possible.It is interesting to compare the event in different wavelengths because they each see different temperatures of plasma. See the transcript for more notes on this.Frames for each wavelength are available on these separate pages: 304, 171, 211, and1700. || ",
            "hits": 332
        }
    ]
}