{
    "count": 8,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 4124,
            "url": "https://svs.gsfc.nasa.gov/4124/",
            "result_type": "Visualization",
            "release_date": "2013-12-05T18:00:00-05:00",
            "title": "The Sun's Magnetic Field",
            "description": "During the course of the approximately 11 year sunspot cycle, the magnetic field of the Sun reverses. The last time this happened was around the year 2000. Using magnetograms from the SOHO/MDI and SDO/HMI instruments, it is possible to examine possible configurations of the magnetic field above the photosphere. These magnetic configurations are important in understanding potential conditions of severe space weather.The magnetic field in this animation is constructed using the Potential Field Source Surface (PFSS) model. The PFSS model is one of the simplest yet realistic models we can explore. Using the solar magnetograms as the 'source surface' of the field, it builds the field structure from the photosphere out to about two solar radii (an altitude of 1 solar radius). These visuals were generated using the SolarSoft package. In this visualization, the white magnetic field lines are considered 'closed'. The move up, and then return to the solar surface. The green and violet lines represenent field lines that are considered 'open'. Green represents positive magnetic polarity, and violet represents negative polarity. These field lines do not connect back to the Sun but with more distant magnetic fields in space. These field lines act as easy 'roads' for the high-speed solar wind. || ",
            "hits": 393
        },
        {
            "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": 3503,
            "url": "https://svs.gsfc.nasa.gov/3503/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/MDI Magnetograms",
            "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 Michelson Doppler Interferometer (MDI) takes images of the Sun at five very narrow wavelength bands and four different polarizations in visible light. For this sequence, the images are processed in a form that reveals the magnetic field strength on the solar photosphere. Other combinations of the images act as white-light images and dopplergrams (which measure the velocity of the solar 'surface').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 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO  For more information, visit the SOHO project page.. || ",
            "hits": 48
        },
        {
            "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": 76
        },
        {
            "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": 33
        },
        {
            "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": 61
        },
        {
            "id": 3211,
            "url": "https://svs.gsfc.nasa.gov/3211/",
            "result_type": "Visualization",
            "release_date": "2005-08-16T12:00:00-04:00",
            "title": "Space Weather Forecasting: Quiet Times Ahead",
            "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a good match (as in this case) indicates that the region will not generate flare events over the next few days. || ",
            "hits": 28
        },
        {
            "id": 3212,
            "url": "https://svs.gsfc.nasa.gov/3212/",
            "result_type": "Visualization",
            "release_date": "2005-08-16T12:00:00-04:00",
            "title": "Space Weather Forecasting: Active Times Ahead",
            "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a bad match (as in this case) indicates that the region will generate flare events over the next few days. || ",
            "hits": 30
        }
    ]
}