{
    "count": 6,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 3809,
            "url": "https://svs.gsfc.nasa.gov/3809/",
            "result_type": "Visualization",
            "release_date": "2011-02-06T11:00:00-05:00",
            "title": "STEREO Achieves Full Solar Coverage: All the Sun. All the Time",
            "description": "When the two STEREO spacecraft move into positions on opposite sides of the Sun, we will have the capability to see a full 360 degrees around the solar sphere (there will probably still be some gaps in visibility near the poles of the Sun). Combined with solar observing satellites near the Earth, such as SDO and SOHO, this coverage will last for about eight years and the STEREO spacecraft move along in their orbits.This movie illustrates the orbital motions of the two STEREO spacecraft relative to the Earth (and noting the positions of the planets Mercury & Venus for reference). The camera occupies a position fixed relative to the Earth and Sun, so the distant starfield appears to spin around the observer. Because the frames are sampled at one per solar day, the Earth does not appear to rotate, but patient observation reveals that the tilt of the planet relative to the Sun, varies throughout the year, with the northern hemisphere tilted towards the Sun in northern hemisphere summer and away from the Sun in northern hemisphere winter. || ",
            "hits": 128
        },
        {
            "id": 3819,
            "url": "https://svs.gsfc.nasa.gov/3819/",
            "result_type": "Visualization",
            "release_date": "2011-02-06T11:00:00-05:00",
            "title": "STEREO Achieves Full Solar Coverage: View from the Farside",
            "description": "When the two STEREO spacecraft move into positions on opposite sides of the Sun, we will have the capability to see a full 360 degrees around the solar sphere (there will probably still be some gaps in visibility near the poles of the Sun). Combined with solar observing satellites near the Earth, such as SDO and SOHO, this coverage will last for about eight years and the STEREO spacecraft move along in their orbits.In this movie, we zoom in towards the Sun, fading from a visible light view to data from the 304 Ångstrom filters aboard SDO and both STEREO spacecraft. We swing the camera around to a view of the side of the Sun NOT visible from the Earth. With the STEREO and SDO data mapped to the sphere representing the Sun, we see the dark sliver of \"No Data\" which slowly shrinks as the STEREO spacecraft move into position 180 degrees apart on opposite sides of the Sun (and 90 degrees from Earth). STEREO data near the edge of the solar disk get stretched when projected onto a sphere and is responsible for the streaking on either side of the dark sliver. These data are sampled roughly six hours apart for each frame of the movie. Slight differenences in the six hour time step creates a slight 'jitter' of the dark sliver. || ",
            "hits": 34
        },
        {
            "id": 3566,
            "url": "https://svs.gsfc.nasa.gov/3566/",
            "result_type": "Visualization",
            "release_date": "2008-12-18T00:00:00-05:00",
            "title": "Multi-Sun Composition",
            "description": "This movie is a composition of multiple solar datasets synchronized in time. The time frame is late October and early November of 2003, the time of some record-breaking solar activity.The background of the movie shows the view of the wide-angle coronagraphs (blue/white), or LASCO instruments, aboard SOHO. They show streams of electrons outbound from the Sun, part of the solar atmosphere. The central green image is the Sun in ultraviolet light from the EIT instrument. Note that flashes of solar flares in the ultraviolet quickly propagate out from the Sun and are visible in LASCO. These events are coronal mass ejections, or CMEs.Overlaid on the upper left is a better view of the EIT ultraviolet image at a wavelength of 195 angstroms (19.5 nanometers).On the lower left, the orange movie is the EIT ultraviolet movie at 304 angstroms (30.4 nanometers).On the upper right is a solar magnetogram, taken by the MDI instrument. The white regions correspond to positive (north) magnetic flux and the dark regions to negative (south) magnetic flux.The colors for the sequences above are not real. They are chosen by convention since the properties recorded by the cameras are not visible to the human eye.The final image on the lower right is also from MDI. It is a combination of several optical wavelengths and is the best representation from SOHO of the Sun in visible light, as we would see it through ground-based telescopes.The movies that are part of this composition are also available individually on the SVS site: Halloween Solar Storms 2003: SOHO/EIT and SOHO/LASCOHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 195 angstromsHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 304 angstromsHalloween Solar Storms 2003: SOHO/MDI ContinuumHalloween Solar Storms 2003: SOHO/MDI Magnetograms || ",
            "hits": 32
        },
        {
            "id": 3501,
            "url": "https://svs.gsfc.nasa.gov/3501/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 Angstroms",
            "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 304 Ångstroms corresponds (30.4 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are  Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 ÅHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ",
            "hits": 62
        },
        {
            "id": 2960,
            "url": "https://svs.gsfc.nasa.gov/2960/",
            "result_type": "Visualization",
            "release_date": "2004-07-08T12:00:00-04:00",
            "title": "Halloween Solar Storms from SOHO/EIT, 304 Angstroms",
            "description": "This view from SOHO/EIT in the 304 angstrom band, shows a group of active regions rotating back into view. This movie is synchronized to play with animation IDs 2959 and 2961. One obvious difference is that solar flares are not as visible at this wavelength than at the 195 angstrom band. The 304 angstrom filter was not used as frequently as the 195 angstrom filter, so this movie has more jumps in its time coverage. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ",
            "hits": 24
        },
        {
            "id": 2766,
            "url": "https://svs.gsfc.nasa.gov/2766/",
            "result_type": "Visualization",
            "release_date": "2003-07-09T12:00:00-04:00",
            "title": "Hi-resolution Solar Views from VAULT: Quiet 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 a relatively calm solar region which still reveals a great deal of activity. || ",
            "hits": 14
        }
    ]
}