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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": 221
        },
        {
            "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": 130
        },
        {
            "id": 4269,
            "url": "https://svs.gsfc.nasa.gov/4269/",
            "result_type": "Visualization",
            "release_date": "2016-10-17T10:00:00-04:00",
            "title": "Various Sun Images for the Hyperwall",
            "description": "The Solar Dynamics Observatory (SDO) provides ultra high-definition imagery of the Sun in 13 different wavelengths, utilizing two imaging instruments, the Atmospheric Imaging Assembly (AIA) instrument and the Helioseismic and Magnetic Imager (HMI). These images were captured by SDO on December 6, 2010. || ",
            "hits": 154
        },
        {
            "id": 4391,
            "url": "https://svs.gsfc.nasa.gov/4391/",
            "result_type": "Visualization",
            "release_date": "2016-01-29T10:00:00-05:00",
            "title": "The Dynamic Solar Magnetic Field",
            "description": "A visualization of the slow changes of the solar magnetic field over the course of four years. || PFSSbasicView_inertial.HD1080i.0400_print.jpg (1024x576) [168.7 KB] || PFSSbasicView_inertial.HD1080i.0400_searchweb.png (180x320) [78.9 KB] || PFSSbasicView_inertial.HD1080i.0400_thm.png (80x40) [5.8 KB] || PFSSbasicView_inertial_1080p30.webm (1920x1080) [18.1 MB] || PFSSbasicView (1920x1080) [128.0 KB] || PFSSbasicView_inertial_1080p30.mp4 (1920x1080) [326.6 MB] || PFSSbasicView_inertial_1080p10.mp4 (1920x1080) [470.2 MB] || PFSSbasicView_HD1080p10.mov (1920x1080) [804.4 MB] || PFSSbasicView_inertial_1080p30.mp4.hwshow [232 bytes] || ",
            "hits": 116
        },
        {
            "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": 318
        },
        {
            "id": 11211,
            "url": "https://svs.gsfc.nasa.gov/11211/",
            "result_type": "Produced Video",
            "release_date": "2013-02-22T10:00:00-05:00",
            "title": "SDO Observes Fast-Growing Sunspot",
            "description": "As magnetic fields on the sun rearrange and realign, dark spots known as sunspots can appear on its surface. Over the course of Feb. 19-20, 2013, scientists watched a giant sunspot form in under 48 hours. It has grown to over six Earth diameters across but its full extent is hard to judge since the spot lies on a sphere not a flat disk.The spot quickly evolved into what's called a delta region, in which the lighter areas around the sunspot, the penumbra, exhibit magnetic fields that point in the opposite direction of those fields in the center, dark area. This is a fairly unstable configuration that scientists know can lead to eruptions of radiation on the sun called solar flares. || ",
            "hits": 83
        },
        {
            "id": 3989,
            "url": "https://svs.gsfc.nasa.gov/3989/",
            "result_type": "Visualization",
            "release_date": "2012-11-20T09:00:00-05:00",
            "title": "The Active Sun from SDO: HMI Magnetogram",
            "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.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it measures the splitting of the spectral lines to determine the intensity of the magnetic field on the solar surface. White represents north magnetic polarity and black represents south magnetic polarity.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": 162
        },
        {
            "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": 10748,
            "url": "https://svs.gsfc.nasa.gov/10748/",
            "result_type": "Produced Video",
            "release_date": "2011-04-21T09:00:00-04:00",
            "title": "SDO: Year One",
            "description": "April 21, 2011 marks the one-year anniversary of the Solar Dynamics Observatory (SDO) First Light press conference, where NASA revealed the first images taken by the spacecraft.In the last year, the sun has gone from its quietest period in years to the activity marking the beginning of solar cycle 24. SDO has captured every moment with a level of detail never-before possible. The mission has returned unprecedented images of solar flares, eruptions of prominences, and the early stages of coronal mass ejections (CMEs). In this video are some of the most beautiful, interesting, and mesmerizing events seen by SDO during its first year.In the order they appear in the video the events are:1. Prominence Eruption from AIA in 304 Ångstroms on March 30, 20102. Cusp Flow from AIA in 171 Ångstroms on February 14, 20113. Prominence Eruption from AIA in 304 Ångstroms on February 25, 20114. Cusp Flow from AIA in 304 Ångstroms on February 14, 20115. Merging Sunspots from HMI in Continuum on October 24-28, 20106. Prominence Eruption and active region from AIA in 304 Ångstroms on April 30, 20107. Solar activity and plasma loops from AIA in 171 Ångstroms on March 4-8, 20118. Flowing plasma from AIA in 304 Ångstroms on April 19, 20109. Active regions from HMI in Magnetogram on March 10, 201110. Filament eruption from AIA in 304 Ångstroms on December 6, 201011. CME start from AIA in 211 Ångstroms on March 8, 201112. X2 flare from AIA in 304 Ångstroms on February 15, 2011 || ",
            "hits": 78
        },
        {
            "id": 10700,
            "url": "https://svs.gsfc.nasa.gov/10700/",
            "result_type": "Produced Video",
            "release_date": "2010-12-15T00:00:00-05:00",
            "title": "Solar Dynamics Observatory countdown",
            "description": "A 10-second countdown using SDO imagery of the sun. The instruments and wavelengths are as follow:10-HMI Magnetogram; 9-AIA 4500; 8-AIA 094; 7-HMI Dopplergram; 6-AIA 171; 5-AIA 171-211-304; 4-AIA 171-211-304; 3-AIA 304; 2-AIA 304; 1-AIA 304 The last 5 seconds of countdown show the large prominence eruption that occured March 30, 2010, just after SDO's sensors were turned on. || ",
            "hits": 30
        },
        {
            "id": 3697,
            "url": "https://svs.gsfc.nasa.gov/3697/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Full Disk View - March 29, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.The black and white region slightly above the center corresponds to a visible sunspot.  Weaker magnetic regions are visible around the disk. || ",
            "hits": 45
        },
        {
            "id": 3705,
            "url": "https://svs.gsfc.nasa.gov/3705/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Sunspot Close-Up - March 29, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This version is a close-up view of a large sunspot group. || ",
            "hits": 36
        },
        {
            "id": 3706,
            "url": "https://svs.gsfc.nasa.gov/3706/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Sunspot Zoom-In - March 29, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This movie zooms-in on a large sunspot group. || ",
            "hits": 28
        },
        {
            "id": 3713,
            "url": "https://svs.gsfc.nasa.gov/3713/",
            "result_type": "Visualization",
            "release_date": "2010-04-21T14:15:00-04:00",
            "title": "SDO/HMI Magnetogram Full Disk View - April 7, 2010",
            "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Gray is zero magnetic field.Notice that the surface magnetic fields reveal much more structure than the white-light images in SDO/HMI Continuum Full Disk View - April 7, 2010. || ",
            "hits": 24
        }
    ]
}