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    "count": 9,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 4560,
            "url": "https://svs.gsfc.nasa.gov/4560/",
            "result_type": "Visualization",
            "release_date": "2017-03-31T09:00:00-04:00",
            "title": "Alfvén Waves - Basic",
            "description": "Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [158.5 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_thm.png (80x40) [4.6 KB] || AlfvenWaveBasic_staticXwide_inertial.HD1080i.0300_web.png (320x180) [71.9 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.mp4 (1920x1080) [34.0 MB] || AlfvenWaveBasic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ",
            "hits": 300
        },
        {
            "id": 4561,
            "url": "https://svs.gsfc.nasa.gov/4561/",
            "result_type": "Visualization",
            "release_date": "2017-03-31T09:00:00-04:00",
            "title": "Alfvén Waves - Kinetic",
            "description": "Kinetic Alfven waves represented by undulation in the magnetic field vector. || AlfvenWaveKinetic_staticXwide_inertial.HD1080i.0300_print.jpg (1024x576) [155.7 KB] || WavesOnly (1920x1080) [128.0 KB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.mp4 (1920x1080) [37.9 MB] || AlfvenWaveKinetic_staticXwide.HD1080i_p30.webm (1920x1080) [4.9 MB] || ",
            "hits": 106
        },
        {
            "id": 4088,
            "url": "https://svs.gsfc.nasa.gov/4088/",
            "result_type": "Visualization",
            "release_date": "2013-09-26T14:00:00-04:00",
            "title": "Reconnection Fronts - What the Models Say...",
            "description": "Mathematical models of Earth's magnetosphere have become increasingly more complex and accurate. They have sufficient detail to illustrate many small-scale phenomena.In this simulation run of the Geospace General Circulation Model (GGCM) we see new details that have been observed by in situ satellites. As the solar wind is deflected around Earth's magnetosphere (the 'bubble' of plasma surrounding Earth held by Earth's magnetic field), plasma flows within the bubble can change. In the graphics below, physical variables such as magnetic field and electric currents are plotted. With these variables, we overlay the net flow of the plasma (arrows), subjected to selection criteria to separate flows of plasma away from Earth and towards Earth. Green arrows are low-speed flows (below about 150 kilometers/second), while red arrows correspond to high-speed plasmal flows (about 300 kilometers/second and higher). || ",
            "hits": 49
        },
        {
            "id": 11309,
            "url": "https://svs.gsfc.nasa.gov/11309/",
            "result_type": "Produced Video",
            "release_date": "2013-09-26T14:00:00-04:00",
            "title": "Several NASA Spacecraft Track Energy Through Space",
            "description": "Taking advantage of an unprecedented alignment of eight satellites through the vast magnetic environment that surrounds Earth in space, including NASA's ARTEMIS and THEMIS, scientists now have comprehensive details of the energy's journey through a process that forms the aurora, called a substorm. Their results showed that small events unfolding over the course of a millisecond can result in energy flows that last up to half an hour and cover an area 10 times larger than Earth.Trying to understand how gigantic explosions on the sun can create space weather effects involves tracking energy from the original event all the way to Earth. It's not unlike keeping tabs on a character in a play with many costume changes, because the energy changes form frequently along its journey: magnetic energy causes eruptions that lead to kinetic energy as particles hurtle away, or thermal energy as the particles heat up. Near Earth, the energy can change through all these various forms once again.Most of the large and small features of substorms take place largely in the portion of Earth's magnetic environment called the magnetotail. Earth sits inside a large magnetic bubble called the magnetosphere. As Earth orbits around the sun, the solar wind from the sun streams past the bubble, stretching it outward into a teardrop. The magnetotail is the long point of the teardrop trailing out to more than 1 million miles on the night side of Earth. The moon orbits Earth much closer, some 240,000 miles away, crossing in and out of the magnetotail. || ",
            "hits": 64
        },
        {
            "id": 2856,
            "url": "https://svs.gsfc.nasa.gov/2856/",
            "result_type": "Visualization",
            "release_date": "2003-11-11T12:00:00-05:00",
            "title": "Model of the Heliosphere Over the Solar Cycle",
            "description": "This magnetohydrodynamical (MHD) model shows how the heliosphere of the Sun might interact with the local interstellar medium (ISM) over the course of a single 11 year solar cycle.  The sun (and the orbit of the Earth) is located in the tiny blue region in the center.  The ISM is moving from left to right.  The solar wind varies from 400 km/s up to 566 km/s and back down to 400 km/s over the cycle in this particular model.  The colors are logarithmically scaled to represent temperature, with blue around 10,000 Kelvins (in the undisturbed ISM and the region immediately around the Sun) and red over 1,000,000 Kelvins (corresponding to the bow shocked region in the plasma).  The green region around the Sun has a radius that varies between 100-200 Astronomical Units. || ",
            "hits": 70
        },
        {
            "id": 117,
            "url": "https://svs.gsfc.nasa.gov/117/",
            "result_type": "Visualization",
            "release_date": "1996-12-12T12:00:00-05:00",
            "title": "Global Hybrid Versus MHD Modeling of the Magnetosphere: Magnetic Potential",
            "description": "This series of animations compares a two-dimensional global hybrid simulation with an magnetohydrodynamic model of the interaction of the solar wind with the Earth's magnetosphere. || ",
            "hits": 20
        },
        {
            "id": 1393,
            "url": "https://svs.gsfc.nasa.gov/1393/",
            "result_type": "Visualization",
            "release_date": "1996-12-12T12:00:00-05:00",
            "title": "Global Hybrid Versus MHD Modeling of the Magnetosphere: Density and Magnetic Field",
            "description": "This series of animations compares a two-dimensional global hybrid simulation with an magnetohydrodynamic model of the interaction of the solar wind with the Earth's magnetosphere. || ",
            "hits": 25
        },
        {
            "id": 86,
            "url": "https://svs.gsfc.nasa.gov/86/",
            "result_type": "Visualization",
            "release_date": "1995-12-19T12:00:00-05:00",
            "title": "2-D Unstructured Mesh Particle-MHD Solar Wind Flow Over the Earth: Magnetic Potential",
            "description": "This series of animations shows a two-dimensional unstructured mesh particle-magnetohydrodynamic solar wind flow simulation of the interaction of the solar wind with the Earth's magnetosphere. || ",
            "hits": 19
        },
        {
            "id": 87,
            "url": "https://svs.gsfc.nasa.gov/87/",
            "result_type": "Visualization",
            "release_date": "1995-12-19T12:00:00-05:00",
            "title": "2-D Unstructured Mesh Particle-MHD Solar Wind Flow Over the Earth:Density and Magnetic Field",
            "description": "This series of animations shows a two-dimensional unstructured mesh particle-magnetohydrodynamic solar wind flow simulation of the interaction of the solar wind with the Earth's magnetosphere. || ",
            "hits": 29
        }
    ]
}