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    "results": [
        {
            "id": 5586,
            "url": "https://svs.gsfc.nasa.gov/5586/",
            "result_type": "Visualization",
            "release_date": "2026-01-20T12:00:00-05:00",
            "title": "Extreme Mass Ratio Black Hole Inspirals (EMRIs)",
            "description": "Shows seven unique black hole inspirals.",
            "hits": 398
        },
        {
            "id": 12604,
            "url": "https://svs.gsfc.nasa.gov/12604/",
            "result_type": "Produced Video",
            "release_date": "2017-06-22T14:00:00-04:00",
            "title": "Scientists Uncover Origins of Dynamic Jets on Sun's Surface",
            "description": "At any given moment, as many as 10 million wild jets of solar material burst from the sun’s surface. They erupt as fast as 60 miles per second, and can reach lengths of 6,000 miles before collapsing. These are spicules, and despite their grass-like abundance, scientists didn’t understand how they form. Now, for the first time, a computer simulation — so detailed it took a full year to run — shows how spicules form, helping scientists understand how spicules can break free of the sun’s surface and surge upward so quickly. This work relied upon high-cadence observations from NASA’s Interface Region Imaging Spectrograph, or IRIS, and the Swedish 1-meter Solar Telescope in La Palma. Together, the spacecraft and telescope peer into the lower layers of the sun’s atmosphere, known as the interface region, where spicules form. The results of this NASA-funded study were published in Science on June 22, 2017 — a special time of the year for the IRIS mission, which celebrates its fourth anniversary in space on June 26.Research: On the generation of solar spicules and Alfvénic waves.Journal: Science, June 22, 2017.Link to paper: http://science.sciencemag.org/content/356/6344/1269.full || ",
            "hits": 55
        },
        {
            "id": 4544,
            "url": "https://svs.gsfc.nasa.gov/4544/",
            "result_type": "Visualization",
            "release_date": "2017-05-26T10:30:00-04:00",
            "title": "2015-2016 El Niño: Daily Sea Surface Temperature Anomaly and Ocean Currents",
            "description": "This visualization shows 2015-2016 El Nino through changes in sea surface temperature and ocean currents.  Blue regions represent colder temperatures and red regions represent warmer temperatures when compared with normal conditions.  Yellow arrows illustrate eastward currents and white arrows are westward currents. || GMAO_elNino_oceanTemperatureAnomaly_currents__1300_print.jpg (1024x576) [175.5 KB] || GMAO_elNino_oceanTemperatureAnomaly_currents__1300_searchweb.png (320x180) [97.1 KB] || GMAO_elNino_oceanTemperatureAnomaly_currents__1300_thm.png (80x40) [6.7 KB] || GMAO_elNino_oceanTemperatureAnomaly_currents_1080p.webm (1920x1080) [163.5 KB] || with_colorbar (3840x2160) [256.0 KB] || GMAO_elNino_oceanTemperatureAnomaly_currents_1080p.mp4 (1920x1080) [159.4 MB] || GMAO_oceanTemperatureAnomaly_withColorbar.mp4 (3840x2160) [166.0 MB] || ",
            "hits": 79
        },
        {
            "id": 4469,
            "url": "https://svs.gsfc.nasa.gov/4469/",
            "result_type": "Visualization",
            "release_date": "2016-06-16T15:00:00-04:00",
            "title": "Dynamic Earth-A New Beginning",
            "description": "The visualization 'Excerpt from \"Dynamic Earth\"' has been one of the most popular visualizations that the Scientific Visualization Studio has ever created.  It's often used in presentations and Hyperwall shows to illustrate the connections between the Earth and the Sun, as well as the power of computer simulation in understanding those connections.There is one part of this visualization, however, that has always seemed a little clumsy to us.  The opening shot is a pullback from the limb of the sun, where the sun is represented by a movie of 304 Angstrom images from the Solar Dynamics Observatory (SDO).  It is difficult to pull back from the limb of a flat sun image and make the sun look spherical, and the problem was made more difficult because the original sun images were in a spherical dome show format.  As a result, the pullback from the sun showed some odd reprojection artifacts.The best solution to this issue was to replace the existing pullout with a new one, one which pulled directly out from the center of the solar disk.  For the new beginning, we chose a series of SDO images in the 171 Angstrom channel that show a visible coronal mass ejection (CME) in the lower right corner of the solar disk.  Although this is not the specific CME that is seen affecting Venus and Earth later in this visualization, its presence links the SDO animation  thematically to the later solar storm.  The SDO images were also brightened considerably and tinted yellow to match the common perception of the Sun as a bright yellow object (even though it is actually white).Please go to the original version of this visualization to see the complete credits and additional details. || ",
            "hits": 90
        },
        {
            "id": 12182,
            "url": "https://svs.gsfc.nasa.gov/12182/",
            "result_type": "Produced Video",
            "release_date": "2016-03-31T13:00:00-04:00",
            "title": "Why Do Raindrop Sizes Matter In Storms?",
            "description": "Not all raindrops are created equal. The size of falling raindrops depends on several factors, including where the cloud producing the drops is located on the globe and where the drops originate in the cloud. For the first time, scientists have three-dimensional snapshots of raindrops and snowflakes around the world from space, thanks to the joint NASA and Japan Aerospace Exploration Agency Global Precipitation Measurement (GPM) mission. With the new global data on raindrop and snowflake sizes this mission provides, scientists can improve rainfall estimates from satellite data and in numerical weather forecast models, helping us better understand and prepare for extreme weather events.Watch this video on the NASA Goddard YouTube Channel. || ",
            "hits": 132
        },
        {
            "id": 4433,
            "url": "https://svs.gsfc.nasa.gov/4433/",
            "result_type": "Visualization",
            "release_date": "2016-02-25T20:00:00-05:00",
            "title": "El Niño: GMAO Daily Sea Surface Temperature Anomaly from 1997/1998 and 2015/2016",
            "description": "This visualization shows how the Sea Surface Temperature Anomaly (SSTA) data and subsurface Temperature Anomaly from the 1997 El Nino year compares to the 2015 El Nino year.  The visualization shows how the 1997 event started from colder-than-average sea surface temperatures – but the 2015 event started with warmer-than-average temperatures not only in the Pacific but also in in the Atlantic and Indian Oceans.This video is also available on our YouTube channel. || SSTcompare1997_2015_0000_print.jpg (1024x576) [87.4 KB] || SSTcompare1997_2015_0000_searchweb.png (320x180) [53.0 KB] || SSTcompare1997_2015_0000_thm.png (80x40) [5.6 KB] || Compare1997_2015_SSTA.mp4 (1920x1080) [28.7 MB] || compare (1920x1080) [0 Item(s)] || Compare1997_2015_SSTA.webm (1920x1080) [1.5 MB] || Compare1997_2015_SSTA.m4v (640x360) [2.5 MB] || Compare1997_2015_SSTA.mp4.hwshow [187 bytes] || ",
            "hits": 109
        },
        {
            "id": 3740,
            "url": "https://svs.gsfc.nasa.gov/3740/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: The View from L1",
            "description": "We start from a position 'behind' the Earth, looking towards the Sun. From this position we see the orbit of the Moon as well as three of the heliospheric 'sentinels' (see \"Sentinels of the Heliosphere\"), ACE, SOHO, and Wind patrolling along 'halo orbits' (Wikipedia) around the Sun-Earth Lagrange Point, L1.The CME (orange isosurface) erupts, heading towards the Earth. The density enhancement of the CME is visible in slice of data in the Earth's orbit plane which provides a better sense of when the CME actually reaches the Earth.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red), 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and make it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 17
        },
        {
            "id": 3741,
            "url": "https://svs.gsfc.nasa.gov/3741/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: The View from Above",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The CME (orange surface) erupts in the direction of the Earth. The orange surface represents a boundary of common pressure differences, which better identifies sharp transitions in pressure common in shocks fronts. The CME clears out particles in the region behind it, called a rarefaction (Wikipedia), visible in the particle density.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 17
        },
        {
            "id": 3742,
            "url": "https://svs.gsfc.nasa.gov/3742/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: A View from the Orbit Plane",
            "description": "We start with a view of the space between the Sun (left) and the Earth (within the small rectangular box on the right), slightly above the ecliptic plane. In the plane of the Earth's orbit, we show a 'slice' of the particle density profile of the solar wind (white to yellow for decreasing particle density). Perpendicular to this, we have another 'slice' of particle density from the Enlil model. The Enlil model extends to 60 degrees above and below the solar equator, and beyond 20 solar radii from the Sun. This gap creates the 'hourglass' empty region around the Sun.The CME (orange surface) erupts in the direction of the Earth. The orange surface represents a boundary of common pressure differences, which better identifies sharp transitions in pressure common in shocks fronts. The CME clears out particles in the region behind it, called a rarefaction (Wikipedia), visible in the particle density.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 34
        },
        {
            "id": 3743,
            "url": "https://svs.gsfc.nasa.gov/3743/",
            "result_type": "Visualization",
            "release_date": "2010-07-08T00:00:00-04:00",
            "title": "Space Weather Event: Close-up on the Earth Environment",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth and move into a position above the Earth's orbital plane with the Earth (geospace) environment in view.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 27
        },
        {
            "id": 3739,
            "url": "https://svs.gsfc.nasa.gov/3739/",
            "result_type": "Visualization",
            "release_date": "2010-07-06T00:00:00-04:00",
            "title": "Space Weather Event: Incoming View",
            "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The nested grid pattern centered on the Earth, provides a sense of scale to the scene. The smallest grid square in the opening view is 1,000 Earth radii on each side. The scale changes by a factor of ten for each step larger or smaller in size.We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth, then move into a position behind the Earth with the Sun visible in the distance.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors correpond to densities of: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, so the value roughly corresponds to the number of atoms per cubic centimeter.This visualization is part of a series of visualizations on space weather modeling. || ",
            "hits": 31
        },
        {
            "id": 10537,
            "url": "https://svs.gsfc.nasa.gov/10537/",
            "result_type": "Produced Video",
            "release_date": "2009-12-08T13:00:00-05:00",
            "title": "Climate in a Box",
            "description": "Recent advances in computer technology and software design make it possible to run massive climate simulations on desktop sized machines. This is a paradigm shift from the need for room sized supercomputers to do important work in climate modelling. In a new initiative, NASA plans to facilitate the wider distribution of desktop sized supercomputers, aimed at democratizing climate research among scientists who might otherwise have been more resource contrained. Included in this video are modelling output runs using GEOS-5 and WRF. || ",
            "hits": 20
        },
        {
            "id": 2641,
            "url": "https://svs.gsfc.nasa.gov/2641/",
            "result_type": "Visualization",
            "release_date": "2002-11-15T12:00:00-05:00",
            "title": "The SC2002 Conference Opening Video",
            "description": "This video introduced the latest in high-performance computing and communications and the best of host city Baltimore to keynote address attendees at the SuperComputing 2002 (SC2002) conference on Tuesday, November 19, 2002. || a002641.00010_print.png (720x480) [597.0 KB] || a002641_pre.jpg (320x262) [15.2 KB] || SVS2002-0034_The_SC2002_Conference_Opening_Video.webmhd.webm (960x540) [106.4 MB] || SVS2002-0034_The_SC2002_Conference_Opening_Video.mov (720x480) [1.6 GB] || a002641.dv (720x480) [1.4 GB] || a002641.mp4 (640x480) [82.9 MB] || a002641.mpg (320x240) [72.2 MB] || ",
            "hits": 18
        }
    ]
}