{
    "count": 9,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 10583,
            "url": "https://svs.gsfc.nasa.gov/10583/",
            "result_type": "Produced Video",
            "release_date": "2010-03-16T00:00:00-04:00",
            "title": "Slices Through the Solar Interior",
            "description": "Scientists using SOHO/MDI data have looked just below the Sun's surface and clearly observed inward flowing material.The strong magnetic fields in the sunspots promote cooling. Cool material contracts and sinks at speeds of up to 3000 miles per hour. This drives an inward flow, like a planet-sized whirlpool, that holds the sunspot together as long as the field is strong enough. Scientists discovered this using a technique called acoustic tomography - a novel method similar to ultrasound diagnostics in medicine that uses sound waves to image structures inside the human body. Scientists also found that sunspots are surprisingly shallow. Conditions in sunspots change from cooler than the surrounding plasma to hotter than the surrounding plasma just 3000 miles below the surface. The cool part of a sunspot has the shape of a stack of two or three nickels. Sunspot magnetic fields block the flows that carry heat energy up from the hot solar interior. That results in higher temperatures below the blockage and cooler temperatures above. The downward flows mentioned above dissipate at the same depth. With these data one cannot get a sharp enough picture to really explain the details. Understanding sunspots is essential for understanding the 11-year solar cycle, solar flare explosions, and huge coronal mass ejections that affect life and society on Earth. || ",
            "hits": 58
        },
        {
            "id": 2950,
            "url": "https://svs.gsfc.nasa.gov/2950/",
            "result_type": "Visualization",
            "release_date": "2004-07-01T12:00:00-04:00",
            "title": "Building a 3-D Coronal Mass Ejection from 2-D Data",
            "description": "Using differences in polarization of light directly from the Sun vs. scattered from the CME electrons, it is possible to derive a distance of matter along the line-of-sight. This version is an early release of animation #2958. || ",
            "hits": 16
        },
        {
            "id": 2958,
            "url": "https://svs.gsfc.nasa.gov/2958/",
            "result_type": "Visualization",
            "release_date": "2004-07-01T12:00:00-04:00",
            "title": "Building a 3-D Coronal Mass Ejection from 2-D Data",
            "description": "Using differences in polarization of light directly from the Sun vs. scattered from the CME electrons, it is possible to derive a distance of matter along the line-of-sight. This version is an enhanced version of animation ID 2950 with a color table enhanced to show fainter regions of the CME. || ",
            "hits": 17
        },
        {
            "id": 2750,
            "url": "https://svs.gsfc.nasa.gov/2750/",
            "result_type": "Visualization",
            "release_date": "2003-09-02T12:00:00-04:00",
            "title": "RHESSI Observes 2.2 MeV Line Emission from a Solar Flare",
            "description": "The solar flare at Active Region 10039 on July 23, 2002 exhibits many exceptional high-energy phenomena including the 2.223 MeV neutron capture line and the 511 keV electron-positron (antimatter) annihilation line. In the animation, the RHESSI low-energy channels (12-25 keV) are represented in red and appears predominantly in coronal loops. The high-energy flux appears as blue at the footpoints of the coronal loops. Violet is used to indicate the location and relative intensity of the 2.2MeV emission. || ",
            "hits": 26
        },
        {
            "id": 2764,
            "url": "https://svs.gsfc.nasa.gov/2764/",
            "result_type": "Visualization",
            "release_date": "2003-07-09T12:00:00-04:00",
            "title": "High Resolution Solar Views From VAULT",
            "description": "This movie illustrates the VAULT camera pointings in relation to the rest of the Sun and views from other instruments. || ",
            "hits": 26
        },
        {
            "id": 2765,
            "url": "https://svs.gsfc.nasa.gov/2765/",
            "result_type": "Visualization",
            "release_date": "2003-07-09T12:00:00-04:00",
            "title": "Hi-resolution Solar Views from VAULT: Active Region",
            "description": "This movie presents the VAULT imagery in the context of simultaneous multi-mission observations.  We zoom-in to a subset of the image which focuses on an active solar region which shows plumes of hot gases rising above the solar surface. || ",
            "hits": 18
        },
        {
            "id": 2304,
            "url": "https://svs.gsfc.nasa.gov/2304/",
            "result_type": "Visualization",
            "release_date": "2001-12-10T11:30:00-05:00",
            "title": "Under the Rotating Sunspot (Layers 0, 1, 2)",
            "description": "Using the SOHO Michelson Doppler Interferometer (MDI), scientists can use a process called Time-Distance helioseismology to determine temperatures and fluid flows under the surface of the Sun. || ",
            "hits": 18
        },
        {
            "id": 2314,
            "url": "https://svs.gsfc.nasa.gov/2314/",
            "result_type": "Visualization",
            "release_date": "2001-12-10T11:30:00-05:00",
            "title": "Temperature and Flows under a Sunspot (Layers 0, 2, 4)",
            "description": "Using the SOHO Michelson Doppler Interferometer (MDI), scientists can use a process called Time-Distance helioseismology to determine temperatures and fluid flows under the surface of the Sun. || ",
            "hits": 22
        },
        {
            "id": 2232,
            "url": "https://svs.gsfc.nasa.gov/2232/",
            "result_type": "Visualization",
            "release_date": "2001-11-06T13:00:00-05:00",
            "title": "SOHO/MDI Investigates Solar Flows Under Sunspots",
            "description": "SOHO/MDI performs a 'sonogram' of the sun, revealing the subsurface temperature profile around a sunspot.  Red isosurfaces denote regions where the sound speed (and temperature) are higher than average while blue isosurfaces directly under the spot illustrate where the sound speed (and temperature) are lower than average. || ",
            "hits": 31
        }
    ]
}