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    "title": "Pole Reversal",
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    "release_date": "2014-01-07T00:00:00-05:00",
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            "title": "For More Information",
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            "description": "See [NASA.gov](http://www.nasa.gov/content/goddard/new-nasa-visualization-shows-suns-magnetic-flip/)",
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                    "name": "Tom Bridgman",
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    "related": [
        {
            "id": 4124,
            "url": "https://svs.gsfc.nasa.gov/4124/",
            "page_type": "Visualization",
            "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. || ",
            "release_date": "2013-12-05T18:00:00-05:00",
            "update_date": "2023-05-03T13:51:22.920202-04:00",
            "main_image": {
                "id": 460247,
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                "filename": "PFSS_0400.jpg",
                "media_type": "Image",
                "alt_text": "Evolution of the solar magnetic field from 1997 to 2013.  Version with time-stamp written in the image file.",
                "width": 1024,
                "height": 1024,
                "pixels": 1048576
            }
        },
        {
            "id": 11429,
            "url": "https://svs.gsfc.nasa.gov/11429/",
            "page_type": "Produced Video",
            "title": "Sun Magnetic Field Flip Live Shots and Media Resources",
            "description": "On Dec. 6, 2013, NASA scientists Alex Young and Holly Gilbert discussed how the sun's magnetic field is in the process of flipping. || ",
            "release_date": "2013-12-05T17:00:00-05:00",
            "update_date": "2023-05-03T13:51:23.098561-04:00",
            "main_image": {
                "id": 460278,
                "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011429/polethumb.jpg",
                "filename": "polethumb.jpg",
                "media_type": "Image",
                "alt_text": "Watch this video on the NASA Goddard YouTube channel.This visualization shows the position of the sun's magnetic fields from January 1997 to December 2013. The field lines swarm with activity: The magenta lines show where the sun's overall field is negative and the green lines show where it is positive. Additional gray lines represent areas of local magnetic variation. \r\rThe entire sun's magnetic polarity, flips approximately every 11 years – though sometimes it takes quite a bit longer – and defines what's known as the solar cycle. The visualization shows how in 1997, the sun shows the positive polarity on the top, and the negative polarity on the bottom. Over the next 16 years, each set of lines is seen to creep toward the opposite pole. By the end of the movie, the flip is almost complete. \r\rAt the height of each magnetic flip, the sun goes through periods of more solar activity, during which there are more sunspots, and more eruptive events such as solar flares and coronal mass ejections, or CMEs. The point in time with the most sunspots is called solar maximum. \r",
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