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    "results": [
        {
            "id": 5543,
            "url": "https://svs.gsfc.nasa.gov/5543/",
            "result_type": "Visualization",
            "release_date": "2025-06-11T10:00:00-04:00",
            "title": "Solar Magnetic Field - from Solar Minimum to Solar Maximum",
            "description": "Visualizations of the solar magnetic field evolution as a potential-field-source-surface model (PFSS) from solar minimum (2019) to solar maximum (2025).",
            "hits": 223
        },
        {
            "id": 5344,
            "url": "https://svs.gsfc.nasa.gov/5344/",
            "result_type": "Visualization",
            "release_date": "2024-10-15T14:00:00-04:00",
            "title": "Solar Cycle 25 - the Solar Magnetic Field from Solar Minimum to Pole Flip",
            "description": "One advantage of long-lived missions like Solar Dynamics Observatory (SDO) is the ability to see slow but significant changes over long periods of time.This view from SDO's Helioseismic and Magnetic Imager (HMI) shows the evolution of sunspots on the solar disk starting from solar minimum (around December 2019) and into the maximum solar activity phase.  The video ends in September 2024, however this maximum phase is expected to continue into 2025.",
            "hits": 574
        },
        {
            "id": 4970,
            "url": "https://svs.gsfc.nasa.gov/4970/",
            "result_type": "Visualization",
            "release_date": "2022-02-25T10:00:00-05:00",
            "title": "The Many Eyes on the Parker Solar Probe Perihelion (February 2022)",
            "description": "This visualization opens with a top-down view, then transtions to an oblique view of the inner solar system with the various solar-observing missions conducting coordinated observations of the plasma environment.   This version displays the imaging instrument camera frustums and solar magnetic field alignments - the 'glyph' version.  A version with just the orbits, no 'glyphs' is available in the [Download Options] menu. || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_print.jpg (1024x576) [123.3 KB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_searchweb.png (320x180) [78.9 KB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HAE.AU.glyphs_CRTT.HD1080.01300_thm.png (80x40) [5.2 KB] || Encounter2022FebTop2Side (1920x1080) [0 Item(s)] || Encounter2022FebTop2Side.glyphs (1920x1080) [0 Item(s)] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.mp4 (1920x1080) [47.0 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.glyphs.HD1080_p30.mp4 (1920x1080) [60.7 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.webm (1920x1080) [9.7 MB] || Encounter2022FebTop2Side (3840x2160) [0 Item(s)] || Encounter2022FebTop2Side.glyphs (3840x2160) [0 Item(s)] || SolarSynergiesPlus.Encounter2022FebTop2Side.UHD2160_p30.mp4 (3840x2160) [143.6 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.glyphs.UHD2160_p30.mp4 (3840x2160) [176.4 MB] || SolarSynergiesPlus.Encounter2022FebTop2Side.HD1080_p30.mp4.hwshow [220 bytes] || ",
            "hits": 91
        },
        {
            "id": 4957,
            "url": "https://svs.gsfc.nasa.gov/4957/",
            "result_type": "Visualization",
            "release_date": "2021-12-14T12:00:00-05:00",
            "title": "Parker Solar Probe: The Origins of Switchbacks",
            "description": "Most of the magnetic field measured at Parker during this time is directed sunward (blue field lines and vectors).  A switchback occurs when the field changes direction almost 180 degrees for a short period of time.  FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows.  The arrows are colored deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line.  The heliospheric magnetic field lines are represented as gold. || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_print.jpg (1024x576) [114.9 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_searchweb.png (320x180) [71.7 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_thm.png (80x40) [4.5 KB] || Switchbacks20181106A (1920x1080) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4 (1920x1080) [25.7 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.webm (1920x1080) [4.4 MB] || Switchbacks20181106A (3840x2160) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.UHD3840_2160p30.mp4 (3840x2160) [100.2 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4.hwshow [229 bytes] || ",
            "hits": 202
        },
        {
            "id": 4958,
            "url": "https://svs.gsfc.nasa.gov/4958/",
            "result_type": "Visualization",
            "release_date": "2021-12-14T12:00:00-05:00",
            "title": "Parker Solar Probe: Crossing the Alfven Surface",
            "description": "Split window view illustrating the orbit of Parker with the orbit trail colored based on the Mach number of the solar wind and the magnetic field lines (represented as gold) connecting back to the Sun.  The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun). || Parker_SolarCloseup.combo.HD1080.00480_print.jpg (1024x576) [121.9 KB] || Parker_SolarCloseup.combo.HD1080.00480_searchweb.png (320x180) [74.1 KB] || Parker_SolarCloseup.combo.HD1080.00480_thm.png (80x40) [5.2 KB] || Parker_SolarCloseup.combo.HD1080 (1920x1080) [0 Item(s)] || Parker_SolarCloseup.combo.HD1080_p30.mp4 (1920x1080) [45.8 MB] || Parker_SolarCloseup.combo.HD1080_p30.webm (1920x1080) [5.6 MB] || Parker_SolarCloseup.combo.UHD2160 (3840x2160) [0 Item(s)] || Parker_SolarCloseup.combo.UHD2160_p30.mp4 (3840x2160) [124.5 MB] || Parker_SolarCloseup.combo.HD1080_p30.mp4.hwshow [202 bytes] || ",
            "hits": 271
        },
        {
            "id": 13715,
            "url": "https://svs.gsfc.nasa.gov/13715/",
            "result_type": "Produced Video",
            "release_date": "2020-09-15T13:00:00-04:00",
            "title": "How To Track The Solar Cycle",
            "description": "A new solar cycle comes roughly every 11 years. Over the course of each cycle, the Sun transitions from relatively calm to active and stormy, and then quiet again; at its peak, the Sun’s magnetic poles flip. Now that the star has passed solar minimum, scientists expect the Sun will grow increasingly active in the months and years to come.Understanding the Sun’s behavior is an important part of life in our solar system. The Sun’s outbursts—including eruptions known as solar flares and coronal mass ejections—can disturb the satellites and communications signals traveling around Earth, or one day, Artemis astronauts exploring distant worlds. Scientists study the solar cycle so we can better predict solar activity. As of 2020, the Sun has begun to shake off the sleep of minimum, which occurred in December 2019, and Solar Cycle 25 is underway. Scientists use several indicators to track solar cycle progress. || ",
            "hits": 324
        },
        {
            "id": 4854,
            "url": "https://svs.gsfc.nasa.gov/4854/",
            "result_type": "Visualization",
            "release_date": "2020-09-15T10:00:00-04:00",
            "title": "Coronal Holes at Solar Minimum and Solar Maximum",
            "description": "A sample of solar coronal holes around the time of the maximum of sunspot activity (April 2014).  Note the polar regions are devoid of coronal holes but a large hole appears in the southern hemisphere. || CoronalHoleMax_AIA193_00150_print.jpg (1024x1024) [173.1 KB] || CoronalHoleMax_AIA193_00150_searchweb.png (320x180) [89.6 KB] || CoronalHoleMax_AIA193_00150_thm.png (80x40) [7.4 KB] || CoronalHoleMax_AIA193_2048p30.mp4 (2048x2048) [61.7 MB] || CoronalHoleMax_AIA193_2048p30.webm (2048x2048) [2.9 MB] || AIA193-Time (4096x4096) [64.0 KB] || AIA193-Frames (4096x4096) [64.0 KB] || CoronalHoleMax_Timestamp (600x100) [64.0 KB] || ",
            "hits": 136
        },
        {
            "id": 4788,
            "url": "https://svs.gsfc.nasa.gov/4788/",
            "result_type": "Visualization",
            "release_date": "2020-02-04T12:00:00-05:00",
            "title": "The Solar Polar Magnetic Field",
            "description": "From our single vantage point of Earth, our view of the Sun is never complete.  While the far-side of the Sun eventually rotates into view, coverage of the Sun's polar regions is never satisfactory as perspective effects either completely block our view or create a distorted view.   We must often resort to computer modeling of these solar polar regions.This visualization presents the Potential Field Source Surface (PFSS) magnetic field model based on solar observations covering the years 2017-2019.  One version also presents the 'hole' in our measurements of the solar polar region.  The region oscillates in size over the course of the year due to the changing perspective created by the tilt of Earth's orbital plane with the solar equator.   In this region, researchers must resort to approximations to build a more complete view of the solar magnetic field.Why is the solar magnetic field in this region important?  Because the combined with the outgoing flow of the solar wind, the magnetic field lines from the polar regions curve up, and then back down to near the Sun's equatorial plane, which is still fairly close to the orbital plane of Earth and other planets in our solar system.  This gives the Sun's polar magnetic field a significant influence on the space weather impacting Earth and crewed and uncrewed assets around the solar system. || ",
            "hits": 94
        },
        {
            "id": 20299,
            "url": "https://svs.gsfc.nasa.gov/20299/",
            "result_type": "Animation",
            "release_date": "2019-12-04T13:00:00-05:00",
            "title": "Parker Science Result animations",
            "description": "On Dec. 4, 2019, four new papers in the journal Nature describe what scientists working with data from NASA's Parker Solar Probe have learned from this unprecedented exploration of our star — and what they look forward to learning next. These findings reveal new information about the behavior of the material and particles that speed away from the Sun, bringing scientists closer to answering fundamental questions about the physics of our star. These animations represent five of those findings. || ",
            "hits": 110
        },
        {
            "id": 4623,
            "url": "https://svs.gsfc.nasa.gov/4623/",
            "result_type": "Visualization",
            "release_date": "2018-04-30T10:00:00-04:00",
            "title": "The Dynamic Solar Magnetic Field with Introduction",
            "description": "This narrated visualization  transitions from a view of the Sun in visible light, to a view in ultraviolet light showing the plasma flowing along solar magnetic structures, to the underlying magnetic field of the solar photosphere, to a model construction of magnetic fieldlines above the photosphere.This video is also available on our YouTube channel. || SolarMagnetism_UHD3840.04000_print.jpg (1024x576) [198.9 KB] || SolarMagnetism_UHD3840.04000_thm.png (80x40) [6.0 KB] || SolarMagnetism_UHD3840.04000_web.png (320x180) [84.1 KB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.webm (1280x720) [33.9 MB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.mov (1280x720) [7.4 GB] || SolarMagnetism_ProRes3_UHD2160_p30_Narrated.mov (3840x2160) [12.8 GB] || ",
            "hits": 132
        },
        {
            "id": 4124,
            "url": "https://svs.gsfc.nasa.gov/4124/",
            "result_type": "Visualization",
            "release_date": "2013-12-05T18:00:00-05:00",
            "title": "The Sun's Magnetic Field",
            "description": "During the course of the approximately 11 year sunspot cycle, the magnetic field of the Sun reverses. The last time this happened was around the year 2000. Using magnetograms from the SOHO/MDI and SDO/HMI instruments, it is possible to examine possible configurations of the magnetic field above the photosphere. These magnetic configurations are important in understanding potential conditions of severe space weather.The magnetic field in this animation is constructed using the Potential Field Source Surface (PFSS) model. The PFSS model is one of the simplest yet realistic models we can explore. Using the solar magnetograms as the 'source surface' of the field, it builds the field structure from the photosphere out to about two solar radii (an altitude of 1 solar radius). These visuals were generated using the SolarSoft package. In this visualization, the white magnetic field lines are considered 'closed'. The move up, and then return to the solar surface. The green and violet lines represenent field lines that are considered 'open'. Green represents positive magnetic polarity, and violet represents negative polarity. These field lines do not connect back to the Sun but with more distant magnetic fields in space. These field lines act as easy 'roads' for the high-speed solar wind. || ",
            "hits": 315
        },
        {
            "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": 113
        }
    ]
}