{
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    "results": [
        {
            "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": 53
        },
        {
            "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": 3978,
            "url": "https://svs.gsfc.nasa.gov/3978/",
            "result_type": "Visualization",
            "release_date": "2012-11-20T09:00:00-05:00",
            "title": "The Active Sun from SDO: 94 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 94 Ångstroms (9.4 nanometers) which highlights a spectral line emitted by iron atoms that have lost 17 electrons (also known as iron-18 or Fe XVIII) at temperatures of 6,000,000 K. Temperatures like this represent regions of the corona during a solar flare.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 instruments. 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 12 second 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": 98
        },
        {
            "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": 66
        },
        {
            "id": 3957,
            "url": "https://svs.gsfc.nasa.gov/3957/",
            "result_type": "Visualization",
            "release_date": "2012-08-24T00:00:00-04:00",
            "title": "Solar Flare from SDO, April 2011 (AIA 94 Å)",
            "description": "The Solar Dynamics Observatory (SDO) observed a large solar flare in April 2011.This visualization was generated using quick-look time resolution (36 seconds) data from the Atmospheric Imaging Assembly (AIA). Two datasets are used, the SDO/AIA 94 Ångstrom wavelength (green color table). This wavelength is in the ultraviolet band of the electromagnetic spectrum. It is not visible to the human eye or to ground-based telescopes so coded colors are used in presentation.It is the source material for \"SDO Year 2 video\". || ",
            "hits": 43
        },
        {
            "id": 3965,
            "url": "https://svs.gsfc.nasa.gov/3965/",
            "result_type": "Visualization",
            "release_date": "2012-07-20T00:00:00-04:00",
            "title": "Impressionist Sun: SDO Source Images",
            "description": "A set of multi-wavelength views of the Sun from SDO provided source and context imagery for the Van Gogh Sun video. This video illustrates how imagery is converted into physical parameters teaching us more about the physical processes taking place in the solar atmosphere. || ",
            "hits": 28
        }
    ]
}