{
    "count": 3,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 10790,
            "url": "https://svs.gsfc.nasa.gov/10790/",
            "result_type": "Produced Video",
            "release_date": "2011-06-09T12:00:00-04:00",
            "title": "Voyager Satellites Find Magnetic Bubbles at Edge of Solar System",
            "description": "The sun's magnetic field spins opposite directions on the north and south poles. These oppositely pointing magnetic fields are separated by a layer of current called the heliospheric current sheet. Due to the tilt of the magnetic axis in relation to the axis of rotation of the Sun, the heliospheric current sheet flaps like a flag in the wind. The flapping current sheet separates regions of oppositely pointing magnetic field, called sectors. As the solar wind speed decreases past the termination shock, the sectors squeeze together, bringing regions of opposite magnetic field closer to each other. The Voyager spacecraft have now found that when the separation of sectors becomes very small, the sectored magnetic field breaks up into a sea of nested \"magnetic bubbles\" in a phenomenon called magnetic reconnection. The region of nested bubbles is carried by the solar wind to the north and south filling out the entire front region of the heliopause and the sector region in the heliosheath.This discovery has prompted a complete revision of what the heliosheath region looks like. The smooth, streamlined look is gone, replaced with a bubbly, frothy outer layer. More animations about the Voyager magnetic bubbles discovery are available. || ",
            "hits": 109
        },
        {
            "id": 10791,
            "url": "https://svs.gsfc.nasa.gov/10791/",
            "result_type": "Produced Video",
            "release_date": "2011-06-09T12:00:00-04:00",
            "title": "Voyager Heliosheath Bubbles Animations",
            "description": "Animations showing the new Voyager findings about the magnetic field in the heliosheath.For more videos and stills about the Voyager magnetic bubbles discovery, go here. || ",
            "hits": 150
        },
        {
            "id": 2856,
            "url": "https://svs.gsfc.nasa.gov/2856/",
            "result_type": "Visualization",
            "release_date": "2003-11-11T12:00:00-05:00",
            "title": "Model of the Heliosphere Over the Solar Cycle",
            "description": "This magnetohydrodynamical (MHD) model shows how the heliosphere of the Sun might interact with the local interstellar medium (ISM) over the course of a single 11 year solar cycle.  The sun (and the orbit of the Earth) is located in the tiny blue region in the center.  The ISM is moving from left to right.  The solar wind varies from 400 km/s up to 566 km/s and back down to 400 km/s over the cycle in this particular model.  The colors are logarithmically scaled to represent temperature, with blue around 10,000 Kelvins (in the undisturbed ISM and the region immediately around the Sun) and red over 1,000,000 Kelvins (corresponding to the bow shocked region in the plasma).  The green region around the Sun has a radius that varies between 100-200 Astronomical Units. || ",
            "hits": 72
        }
    ]
}