{
    "count": 9,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 11277,
            "url": "https://svs.gsfc.nasa.gov/11277/",
            "result_type": "Produced Video",
            "release_date": "2013-07-09T00:00:00-04:00",
            "title": "Hot Lines",
            "description": "Magnetic field lines dance above the surface of the sun. Called coronal loops, these lines are difficult to observe from afar, since they are invisible. Scientists can observe them in two ways: by watching the visible solar material that flows along the lines or by modeling them using computer simulations. Studying these formations help us understand the way energy travels on and around the sun. The Solar and Heliospheric Observatory, or SOHO, is a sun-observing spacecraft that can measure and depict distortions in the sun’s magnetic field. Using data collected by the spacecraft, scientists created a virtual, 3D model of the field lines. Watch the video to explore the loops. || ",
            "hits": 13
        },
        {
            "id": 3591,
            "url": "https://svs.gsfc.nasa.gov/3591/",
            "result_type": "Visualization",
            "release_date": "2009-04-09T00:00:00-04:00",
            "title": "STEREO Visits the Lagrange Points - L4 and L5",
            "description": "The two STEREO spacecraft orbit the Sun in orbits slightly different from the Earth. STEREO A orbits between the Earth and the Sun, while STEREO-B orbits beyond the Earth and the Sun. As a result, relative to the Earth, STEREO-A appears to move ahead of the Earth, while STEREO-B falls behind the Earth, in their motion around the Sun.In this configuration, the two spacecraft are now passing near the two stable Lagrange Points, L4 and L5, of the Earth-Sun system. The STEREO spacecraft are imaging these regions in the hopes of finding material that might have been left over from the original formation of the Solar System.Revision Note: April 15, 2009:It was pointed out that L4 and L5 were reversed in the initial release of this visualization. These animations and stills were revised to reflect the corrections. We apologize for any inconvenience. || ",
            "hits": 223
        },
        {
            "id": 3405,
            "url": "https://svs.gsfc.nasa.gov/3405/",
            "result_type": "Visualization",
            "release_date": "2007-03-01T00:00:00-05:00",
            "title": "STEREO Panoramic View",
            "description": "The STEREO mission presents a new view of the space between the Earth and the Sun.This view from the STEREO-A satellite, demonstrates the broad range of sky coverage by the five cameras of the SECCHI instrument. || ",
            "hits": 59
        },
        {
            "id": 3406,
            "url": "https://svs.gsfc.nasa.gov/3406/",
            "result_type": "Visualization",
            "release_date": "2007-03-01T00:00:00-05:00",
            "title": "STEREO Coronal Mass Ejection:  From the EUVI to HI-2",
            "description": "This movie collects imagery from SOHO and STEREO-A of a coronal mass ejection (CME) during January of 2007. The instruments in this view, from left to right, are STEREO/HI-1, STEREO/HI-2, SOHO/LASCO/C3, SOHO/LASCO/C2, and STEREO/EUVI. The Heliospheric Imager, HI-2, shows some of the tail of comet McNaught. The dark trapezoidal shape on the left edge of the image in HI-2 is the Earth occulter which will block out the disk of the Earth when it moves into view (since the planet will appear so bright as to saturate the detectors). Due to ongoing work with the STEREO coronagraphs, COR1 and COR2, the SOHO/LASCO coronagraphs are used for this movie. The blue Sun in the center of the coronagraphs is STEREO/EUVI ultraviolet images.There is a 22 hour gap in the data coverage for HI-2 which creates the appearance of a jump in the playback.These are not standard images but are called 'running difference' images which highlight changes in the view. White pixels correspond to increases in brightness, while dark pixels reflect a decrease in brightness, with respect to the immediately previous image.'Running differencing' generates some unusual effects. For example, the mottled background is created by the motion of the stars through the field-of-view as the spacecraft pointing direction slowly changes (the Andromeda galaxy is the oblong 'smudge' near the upper left corner). The planets Venus (right edge of HI-2) and Mercury are visible (near center of HI-1), their column of pixels saturated due to their brightness.STEREO: Solar TErrestrial RElations ObservatorySOHO: SOlar Heliospheric ObservatoryLASCO: Large Angle and Spectrometric CoronagraphEUVI: Extreme UltraViolet Imager || ",
            "hits": 53
        },
        {
            "id": 3407,
            "url": "https://svs.gsfc.nasa.gov/3407/",
            "result_type": "Visualization",
            "release_date": "2007-03-01T00:00:00-05:00",
            "title": "STEREO's Extreme UltraViolet Imager (EUVI)",
            "description": "At a pixel resolution of 2048x2048, the STEREO EUVI instrument provides views of the Sun in ultraviolet light that rivals the full-disk views of SOHO/EIT. This image is through the 171 angstrom (ultraviolet) filter which is characteristic of iron ions (missing eight and nine electrons) at 1 million degrees. There is a short data gap in the latter half of the movie that creates a freeze and then jump in the data view.  STEREO: Solar TErrestrial RElations Observatory SOHO: SOlar Heliospheric Observatory EIT: Extreme ultraviolet Imaging Telescope EUVI: Extreme UltraViolet Imager || ",
            "hits": 80
        },
        {
            "id": 3364,
            "url": "https://svs.gsfc.nasa.gov/3364/",
            "result_type": "Visualization",
            "release_date": "2007-02-07T00:00:00-05:00",
            "title": "STEREO's Routes to Solar Orbits",
            "description": "The two STEREO spacecraft, A (red path) and B (yellow path), are launched from the Earth into a highly eccentric orbit with an apogee that reaches the orbit of the Moon. Once in this orbit, the trajectories are adjusted so they can receive gravity-assists from the Moon. The gravity assist will send them both into heliocentric orbits, one spacecraft ahead of the Earth and the other behind the Earth.This trajectory was generated using a spacecraft ephemeris generated shortly after launch. || ",
            "hits": 102
        },
        {
            "id": 3346,
            "url": "https://svs.gsfc.nasa.gov/3346/",
            "result_type": "Visualization",
            "release_date": "2006-03-30T00:00:00-05:00",
            "title": "Grand Tour of the Coronal Loops Model",
            "description": "This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT standard color table. || ",
            "hits": 64
        },
        {
            "id": 3286,
            "url": "https://svs.gsfc.nasa.gov/3286/",
            "result_type": "Visualization",
            "release_date": "2005-10-27T00:00:00-04:00",
            "title": "Flight through the Coronal Loops",
            "description": "Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT 'standard color table'. || ",
            "hits": 30
        },
        {
            "id": 3287,
            "url": "https://svs.gsfc.nasa.gov/3287/",
            "result_type": "Visualization",
            "release_date": "2005-10-27T00:00:00-04:00",
            "title": "Rotating Tour of Solar Coronal Loops",
            "description": "A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 angstroms, the filter wavelength of SOHO/EIT. || ",
            "hits": 42
        }
    ]
}