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    "title": "Solar Vibrations",
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            "description": "Material inside the sun is constantly on the move. This movement can produce pressure waves that travel through the sun and cause its surface to vibrate. Solar physicists have given a name to the study of these motions that were first observed in the 1970s—helioseismology. Just as seismic waves can be used to visualize Earth’s interior, scientists can use pressure waves to infer information about the sun’s inner structure. Since 2010, the Helioseismic and Magnetic Imager (HMI) instrument aboard NASA’s Solar Dynamics Observatory (SDO) spacecraft has observed oscillating solar material on the sun's surface layer, the photosphere. Thanks to the instrument, scientists have been able to hone their models of how material circulates within the sun, helping them explore how regions of active magnetism ramp up and erupt as solar flares and coronal mass ejections. Watch the video to see a time-lapse of SDO images that shows shifting material on the sun’s surface.",
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    "related": [
        {
            "id": 3988,
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            "page_type": "Visualization",
            "title": "The Active Sun from SDO: HMI Intensity",
            "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it shows the solar photosphere in visible light.This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ",
            "release_date": "2012-11-20T09:00:00-05:00",
            "update_date": "2025-02-02T22:08:41.109953-05:00",
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                "filename": "SDOHMIintensity_Jewelbox_stand.HD1080i.00100.jpg",
                "media_type": "Image",
                "alt_text": "Stand-alone movies of HMI intensity imagery.",
                "width": 1920,
                "height": 1080,
                "pixels": 2073600
            }
        },
        {
            "id": 3990,
            "url": "https://svs.gsfc.nasa.gov/3990/",
            "page_type": "Visualization",
            "title": "The Active Sun from SDO: HMI Dopplergram",
            "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it measures the shifting of the spectral lines to determine the velocity of gas flows on the solar surface. This spectral line shift is due to the Doppler effect (Wikipedia). Blue represents motion towards the observer. Red indicates motion away from the observer. For the images below, the color is dominated by the solar rotation, so the solar limb on the right is moving away from us (and therefore red) while the left limb is moving towards us (and therefore blue). Motions on the solar surface generate the rippling in the color and you can see evidence of surface flows around the sunspot near the left limb. This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ",
            "release_date": "2012-11-20T09:00:00-05:00",
            "update_date": "2025-02-02T22:08:49.145735-05:00",
            "main_image": {
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                "filename": "SDOHMIdoppler_Jewelbox_stand.HD1080i.00100.jpg",
                "media_type": "Image",
                "alt_text": "Stand-alone movie of the HMI dopplergrams",
                "width": 1920,
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                "pixels": 2073600
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        {
            "id": 3714,
            "url": "https://svs.gsfc.nasa.gov/3714/",
            "page_type": "Visualization",
            "title": "SDO/HMI Dopplergram Sunspot Close-Up - March 29, 2010",
            "description": "The dopplergram from SDO/HMI data shows the velocity of solar material on the line-of-sight. White pixels are moving away from the camera and black pixels are moving towards the camera. || ",
            "release_date": "2010-04-21T14:15:00-04:00",
            "update_date": "2023-05-03T13:54:17.011725-04:00",
            "main_image": {
                "id": 493383,
                "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003700/a003714/SDOHMIdoppler29March050.jpg",
                "filename": "SDOHMIdoppler29March050.jpg",
                "media_type": "Image",
                "alt_text": "This movie is a dopplergram of the sunspot group of March 29, 2010 taken with HMI.",
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            }
        }
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