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    "results": [
        {
            "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": 85
        },
        {
            "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": 157
        },
        {
            "id": 3999,
            "url": "https://svs.gsfc.nasa.gov/3999/",
            "result_type": "Visualization",
            "release_date": "2012-10-26T00:00:00-04:00",
            "title": "The View from SDO: The August 31, 2012 Filament Eruption",
            "description": "The Solar Dynamics Observatory (SDO) observed a large filament eruption on August 31, 2012. This visualization was generated using high time resolution (12 seconds) data from the Atmospheric Imaging Assembly (AIA). Two datasets are used, the SDO/AIA 304 Ångstrom wavelength (orange color table) and the 171 Ångstrom wavelength (gold color table). These are wavelengths in the ultraviolet band of the electromagnetic spectrum. They are not visible to the human eye or to ground-based telescopes so coded colors are used in presentation.It is the source material for \"August 31, 2012 Magnificent CME\" visualization. || ",
            "hits": 90
        },
        {
            "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": 67
        },
        {
            "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": 23
        },
        {
            "id": 3828,
            "url": "https://svs.gsfc.nasa.gov/3828/",
            "result_type": "Visualization",
            "release_date": "2011-12-07T00:00:00-05:00",
            "title": "Solar Dynamics Observatory - Atmospheric Imaging Assembly",
            "description": "The Sun's activity increases as we enter solar cycle 24. But even several years away from the peak, the Sun in ultraviolet light shows a variety of activity.This visualization consists of eight hours of SDO AIA imagery from the 30.4 nanometer filter (304 Ångstroms). This sequence plays at the full time cadence of the AIA instrument - one image every twelve seconds of real time - and showing thirty images per second on playback. || ",
            "hits": 188
        },
        {
            "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": 70
        },
        {
            "id": 3496,
            "url": "https://svs.gsfc.nasa.gov/3496/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Plasma Flows",
            "description": "In this visualization, we illustrate the fluid flows in the Sun which drive the solar magnetic dynamo. The flows can be considered as a combination of two components, a toroidal component and a meridional component. The toroidal flow corresponds to the rotational motion of the Sun. In the cut-away view, this motion is represented by the streaking flow vectors. The color code of the cross-section on the right-hand side illustrates the rotational period of this flow. Here we see that flow near the equator (in violet) takes about 24.5 days to make it all the way around the Sun. As we move to higher latitudes, we see that the flow gets steadily slower, increasing the time it takes to go around the Sun to as much as 34 days (in red) near the poles. A non-uniform fluid flow such as this is known as differential rotation. This motion in the interior can be measured at the solar surface through techniques of helioseismology.Deeper into the Sun, we see the different colors of the outer layers transition to a solid color (olive green). This transition point is called the tachocline. It is the boundary between the outer zone of the Sun where thermal energy is transferred by convection (the convective zone), and the inner region of the Sun where thermal energy is transferred by radiation (the radiative zone). The radiative zone is believed to rotate as a solid body with a period of about 28 days in this model.The yellow and white center in this model represents the solar radiative zone.In the cross-section on the left-side, we represent the other component of the flow, called the meridional flow, which moves plasma between the equator and the polar regions.These flows of solar plasma are used as input data for dynamo modeling (see The Solar Dynamo: Toroidal and Poloidal Fields and The Solar Dynamo: Toroidal and Radial Fields.) || ",
            "hits": 114
        },
        {
            "id": 3521,
            "url": "https://svs.gsfc.nasa.gov/3521/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Toroidal and Poloidal Magnetic Fields",
            "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, the field intensity represented by colors on the right-hand cross-section, and the poloidal magnetic potential field, represented by colors on the left-hand cross-section. The poloidal magnetic potential is a scalar quantity that contains information about the radial and latitudinal magnetic field vectors. To see the radial magnetic field, see The Solar Dynamo: Toroidal and Radial Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time. Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field. Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator as the solar cycle progresses. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ",
            "hits": 137
        },
        {
            "id": 3583,
            "url": "https://svs.gsfc.nasa.gov/3583/",
            "result_type": "Visualization",
            "release_date": "2008-08-19T00:00:00-04:00",
            "title": "The Solar Dynamo: Toroidal and Radial Magnetic Fields",
            "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, intensities represented by color on the right-hand cross-section, and the radial magnetic field, represented on the left-hand cross-section. To see the poloidal magnetic vector potential, see The Solar Dynamo: Toroidal and Poloidal Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time.Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field.Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ",
            "hits": 97
        },
        {
            "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": 79
        }
    ]
}