The Extreme Ultraviolet (EUV) Variability Experiment (EVE) measures extreme ultraviolet emission from the solar chromosphere, transition region and corona. This radiation is mostly absorbed in Earth's upper atmosphere and influences Earth's climate.
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. This differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting.", "items": [], "extra_data": {} }, { "id": 347580, "url": "https://svs.gsfc.nasa.gov/4009/#media_group_347580", "widget": "Video player", "title": "", "caption": "", "description": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "items": [ { "id": 315069, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472818, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE.01554.png", "filename": "SDOEVE.01554.png", "media_type": "Image", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 315067, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472814, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE_2011_268_HD1080_web.png", "filename": "SDOEVE_2011_268_HD1080_web.png", "media_type": "Image", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 315068, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472815, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE.00100_thm.png", "filename": "SDOEVE.00100_thm.png", "media_type": "Image", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 80, "height": 40, "pixels": 3200 } }, { "id": 315063, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472812, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE_2011_268_HD1080.mov", "filename": "SDOEVE_2011_268_HD1080.mov", "media_type": "Movie", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 315064, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472816, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE_2011_268_HD1080.mp4", "filename": "SDOEVE_2011_268_HD1080.mp4", "media_type": "Movie", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 315066, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472813, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/frames/1920x1080_16x9_30p/", "filename": "1920x1080_16x9_30p", "media_type": "Frames", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 315070, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472819, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE_2011_268_HD1080.webmhd.webm", "filename": "SDOEVE_2011_268_HD1080.webmhd.webm", "media_type": "Movie", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 960, "height": 540, "pixels": 518400 } }, { "id": 315065, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 472817, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004009/SDOEVE_2011_268_iPod.m4v", "filename": "SDOEVE_2011_268_iPod.m4v", "media_type": "Movie", "alt_text": "A plot of EVE spectral data with time. The EVE data (yellow) overlays the WHI 2008 reference spectrum of the Sun. Markers along the bottom indicate wavelength coverage for other SDO instruments such as EVE/SAM imager, AIA, and HMI.", "width": 640, "height": 360, "pixels": 230400 } } ], "extra_data": {} } ], "studio": "SVS", "funding_sources": [ "NASA Heliophysics" ], "credits": [ { "role": "Animator", "people": [ { "name": "Tom Bridgman", "employer": "Global Science and Technology, Inc." } ] }, { "role": "Producer", "people": [ { "name": "Scott Wiessinger", "employer": "USRA" }, { "name": "Genna Duberstein", "employer": "USRA" } ] }, { "role": "Scientist", "people": [ { "name": "Phil Chamberlin", "employer": "NASA/GSFC" } ] } ], "missions": [ "SDO" ], "series": [ "SDO Jewelbox" ], "tapes": [], "papers": [], "datasets": [ { "name": "Ultraviolet Spectral Solar Irradiance", "common_name": "SSI", "platform": "SDO", "sensor": "EVE", "type": "Observed Data", "organizations": [], "description": "", "credit": "", "url": "", "date_range": null }, { "name": "Solar Spectral Irradiance Reference Spectra", "common_name": "WHI 2008", "platform": null, "sensor": null, "type": "Data Compilation", "organizations": [], "description": "", "credit": "", "url": "", "date_range": null } ], "nasa_science_categories": [ "Sun" ], "keywords": [ "Earth Science", "Heliophysics", "Hyperwall", "SDO", "Solar Activity", "Solar Dynamics Observatory", "Solar Ultraviolet", "Sun-earth Interactions" ], "recommended_pages": [], "related": [ { "id": 3978, "url": "https://svs.gsfc.nasa.gov/3978/", "page_type": "Visualization", "title": "The Active Sun from SDO: 94 Ångstroms", "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.This movie is generated for a wavelength of 94 Ångstroms (9.4 nanometers) which highlights a spectral line emitted by iron atoms that have lost 17 electrons (also known as iron-18 or Fe XVIII) at temperatures of 6,000,000 K. Temperatures like this represent regions of the corona during a solar flare.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 instruments. 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 12 second 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": "2023-11-14T00:02:59.476396-05:00", "main_image": { "id": 472643, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003978/SDOAIA094A_Jewelbox_stand.HD1080i.01000.jpg", "filename": "SDOAIA094A_Jewelbox_stand.HD1080i.01000.jpg", "media_type": "Image", "alt_text": "Stand-alone full-disk movies of AIA 94Ångstrom imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3979, "url": "https://svs.gsfc.nasa.gov/3979/", "page_type": "Visualization", "title": "The Active Sun from SDO: 131 Ångstroms", "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.This movie is generated for a wavelength of 131 Ångstroms (13.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 19 and 22 electrons (also known as iron-20 or Fe XX; and iron-23 or FeXXIII) at temperatures of 10,000,000 K. Temperatures like this represent material in a solar flare.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": "2023-11-14T00:03:01.861062-05:00", "main_image": { "id": 472601, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003979/SDOAIA131A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA131A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 Movie of AIA 131Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3980, "url": "https://svs.gsfc.nasa.gov/3980/", "page_type": "Visualization", "title": "The Active Sun from SDO: 171 Ångstroms", "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.This movie is generated for a wavelength of 171 Ångstroms (17.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 8 electrons (also known as iron-9 or Fe IX) at temperatures of 600,000 K. Temperatures like this show the quiet corona and magnetic structures like coronal loops.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": "2023-11-14T00:03:04.262505-05:00", "main_image": { "id": 472653, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003980/SDOAIA171A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA171A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 171Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3981, "url": "https://svs.gsfc.nasa.gov/3981/", "page_type": "Visualization", "title": "The Active Sun from SDO: 193 Ångstroms", "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.This movie is generated for a wavelength of 193 Ångstroms (19.3 nanometers) which highlights a spectral line emitted by iron atoms that have lost 11 electrons (also known as iron-12 or Fe XII) at temperatures of 1,000,000 K as well as iron atoms that have lost 23 electrons (also known as iron-24 or FeXXIV) at temperatures of 20,000,000K. The former represents a slightly higher region of the corona and the latter represents the much hotter material of a solar flare. This wavelength also makes coronal holes (which appear as dark regions near the solar surface) more visible.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": "2023-11-14T00:03:07.145305-05:00", "main_image": { "id": 472670, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003981/SDOAIA193A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA193A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 193 Å imagery.", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3982, "url": "https://svs.gsfc.nasa.gov/3982/", "page_type": "Visualization", "title": "The Active Sun from SDO: 211 Ångstroms", "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.This movie is generated for a wavelength of 211 Ångstroms (21.1 nanometers) which highlights a spectral line emitted by iron atoms that have lost 13 electrons (also known as iron-14 or Fe XIV) at temperatures of 2,000,000 K. These images show hotter, active regions in the sun's corona.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": "2023-11-14T00:03:09.726467-05:00", "main_image": { "id": 472618, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003982/SDOAIA211A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA211A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 211 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3983, "url": "https://svs.gsfc.nasa.gov/3983/", "page_type": "Visualization", "title": "The Active Sun from SDO: 304 Ångstroms", "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.This movie is generated for a wavelength of 304 Ångstroms (30.4 nanometers) which highlights a spectral line emitted by helium atoms that have lost 1 electron (also known as helium-2 or He II) at temperatures of 50,000 K. This light is emitted from the upper transition region and the chromosphere. Solar prominences are readily visible at this wavelength.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": "2023-11-14T00:03:11.895798-05:00", "main_image": { "id": 472687, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003983/SDOAIA304A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA304A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 304 ", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3984, "url": "https://svs.gsfc.nasa.gov/3984/", "page_type": "Visualization", "title": "The Active Sun from SDO: 335 Ångstroms", "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.This movie is generated for a wavelength of 335 Ångstroms (33.5 nanometers) which highlights a spectral line of iron that has lost 15 electrons (also known as iron-16 or Fe XVI) at temperatures of 2,500,000 K. These images show active regions in the corona.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": "2023-11-14T00:03:13.805600-05:00", "main_image": { "id": 472584, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003984/SDOAIA335A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA335A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 335 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3985, "url": "https://svs.gsfc.nasa.gov/3985/", "page_type": "Visualization", "title": "The Active Sun from SDO: 1600 Ångstroms", "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.This movie is generated for a wavelength of 1600 Ångstroms (160.0 nanometers) which highlights a spectral line of carbon that has lost 3 electrons (also known as carbon-4 or C-IV) at temperatures of 10,000 K. C IV at these temperatures is present in what's called the transition region between the sun's surface and the lowest levels of the sun's atmosphere, the chromosphere.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": "2023-11-14T00:03:16.371780-05:00", "main_image": { "id": 472704, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003985/SDOAIA1600A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA1600A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 1600 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3986, "url": "https://svs.gsfc.nasa.gov/3986/", "page_type": "Visualization", "title": "The Active Sun from SDO: 1700 Ångstroms", "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.This movie is generated for a wavelength of 1700 Ånstroms (170.0 nanometers) which is in the ultraviolet band showing the lower level of the Sun's atmosphere, called the chromosphere.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": "2023-11-14T00:03:18.263749-05:00", "main_image": { "id": 472721, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003986/SDOAIA1700A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA1700A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 1700 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3987, "url": "https://svs.gsfc.nasa.gov/3987/", "page_type": "Visualization", "title": "The Active Sun from SDO: 4500 Ångstroms", "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.This movie is generated for a wavelength of 4500 Ångstroms (450.0 nanometers) which corresponds to visible light, showing the Sun's visible surface, or photosphere. This wavelength can also be seen from the surface of the Earth, though not with the clarity possible from SDO. The dark regions on the left side are sunspots (Wikipedia) - essentially magnetic storms in the photosphere.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": "2023-11-14T00:03:20.041371-05:00", "main_image": { "id": 472738, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003987/SDOAIA4500A_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOAIA4500A_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of AIA 4500 Å imagery", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 3988, "url": "https://svs.gsfc.nasa.gov/3988/", "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": "2023-11-14T00:03:22.041480-05:00", "main_image": { "id": 472755, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003988/SDOHMIintensity_Jewelbox_stand.HD1080i.00100.jpg", "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": 3989, "url": "https://svs.gsfc.nasa.gov/3989/", "page_type": "Visualization", "title": "The Active Sun from SDO: HMI Magnetogram", "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 splitting of the spectral lines to determine the intensity of the magnetic field on the solar surface. White represents north magnetic polarity and black represents south magnetic polarity.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": "2023-11-14T00:03:24.205593-05:00", "main_image": { "id": 472772, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003989/SDOHMImagnetogram_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOHMImagnetogram_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone HD1080 movie of the HMI magnetograms.", "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": "2023-11-14T00:03:26.674862-05:00", "main_image": { "id": 472789, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003990/SDOHMIdoppler_Jewelbox_stand.HD1080i.00100.jpg", "filename": "SDOHMIdoppler_Jewelbox_stand.HD1080i.00100.jpg", "media_type": "Image", "alt_text": "Stand-alone movie of the HMI dopplergrams", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 4008, "url": "https://svs.gsfc.nasa.gov/4008/", "page_type": "Visualization", "title": "SDO Jewelbox: The Many Eyes of SDO", "description": "5x3 Layout view. This version has the imagery organized in order of increasing wavelength, from upper left to lower right for AIA. The HMI products occupy the bottom row. || SDOJewelbox_5x3.0100.jpg (2400x810) [317.7 KB] || SDOJewelbox_5x3.0100_web.png (320x108) [28.9 KB] || SDOJewelbox_5x3.0100_thm.png (80x40) [3.7 KB] || SDOJewelbox_5x3.0100_searchweb.png (320x180) [29.2 KB] || SDOJewelbox_5x3.webmhd.webm (960x540) [3.3 MB] || SDOJewelbox_5x3.mov (2400x810) [91.5 MB] || SDOJewelbox_5x3.mp4 (2400x810) [91.5 MB] || frames/2400x810_80x27_30p/ (2400x810) [128.0 KB] || ", "release_date": "2012-11-20T09:00:00-05:00", "update_date": "2023-11-14T00:03:36.746415-05:00", "main_image": { "id": 472810, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a004000/a004008/SDOJewelbox_3x3.0100.jpg", "filename": "SDOJewelbox_3x3.0100.jpg", "media_type": "Image", "alt_text": "3x3 Layout view. This version is a subset of SDO filters. HMI imagery occupies the top row. EVE data is in the center. Selected AIA wavelengths other spots.", "width": 1920, "height": 1080, "pixels": 2073600 } } ], "sources": [], "products": [], "newer_versions": [], "older_versions": [], "alternate_versions": [] }