{
    "count": 2,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 3548,
            "url": "https://svs.gsfc.nasa.gov/3548/",
            "result_type": "Visualization",
            "release_date": "2008-09-10T00:00:00-04:00",
            "title": "Comparison: Solar Minimum from SOHO/EIT",
            "description": "This is a short movie of the Sun at the minimum of solar activity. This images are collected in ultraviolet light (a wavelength of 195 Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, few to now sunspots would be visible.At solar minimum, we see few bright active regions. The mottled look is from small 'hot spots' which last less than 48 hours. There are dark regions at the top and bottom of the Sun (corresponding to the north and south solar poles) created by solar magnetic field lines that connect to the interstellar magnetic field. A similar dark region, below the solar equator, is called a coronal hole, where open magnetic field lines enable particles to stream away at high speeds. || ",
            "hits": 32
        },
        {
            "id": 3549,
            "url": "https://svs.gsfc.nasa.gov/3549/",
            "result_type": "Visualization",
            "release_date": "2008-09-10T00:00:00-04:00",
            "title": "Comparison: Solar Maximum from SOHO/EIT",
            "description": "A short movie of the Sun at maximum solar activity as seen in ultraviolet light. These images are collected in ultraviolet light (a wavelength of 195Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, the bright white regions in these images would probably correspond to sunspots.At solar maximum, we see many bright active regions which tend to form in bands in the northern and southern hemispheres. Many of the active regions may eventually launch solar flares or coronal mass ejections (CME). || ",
            "hits": 39
        }
    ]
}