{ "count": 44, "next": null, "previous": null, "results": [ { "id": 5577, "url": "https://svs.gsfc.nasa.gov/5577/", "result_type": "Animation", "release_date": "2025-11-20T09:00:00-05:00", "title": "SDO Sun This Week", "description": "This visualization shows SDO AIA-304 imagery from the past 7 days with a color table and image processing applied. Archive folders are provided in the Download menu.", "hits": 0 }, { "id": 5524, "url": "https://svs.gsfc.nasa.gov/5524/", "result_type": "Interactive", "release_date": "2025-05-22T08:00:59-04:00", "title": "\"Snap It!\" Solar Eclipse Photography Game", "description": "The Traveler needs your help! They have come to Earth to study an event we call a total solar eclipse. Can you help the Traveler snap photos of an eclipse?", "hits": 78 }, { "id": 4269, "url": "https://svs.gsfc.nasa.gov/4269/", "result_type": "Visualization", "release_date": "2016-10-17T10:00:00-04:00", "title": "Various Sun Images for the Hyperwall", "description": "The Solar Dynamics Observatory (SDO) provides ultra high-definition imagery of the Sun in 13 different wavelengths, utilizing two imaging instruments, the Atmospheric Imaging Assembly (AIA) instrument and the Helioseismic and Magnetic Imager (HMI). These images were captured by SDO on December 6, 2010. || ", "hits": 164 }, { "id": 12144, "url": "https://svs.gsfc.nasa.gov/12144/", "result_type": "Produced Video", "release_date": "2016-02-12T09:00:00-05:00", "title": "SDO: Year 6", "description": "This ultra-high definition (3840x2160) video shows the sun in the 171 angstrom wavelength of extreme ultraviolet light. It covers a time period of January 2, 2015 to January 28, 2016 at a cadence of one frame every hour, or 24 frames per day. This timelapse is repeated with narration by solar scientist Nicholeen Viall and contains close-ups and annotations. 171 angstrom light highlights material around 600,000 Kelvin and shows features in the upper transition region and quiet corona of the sun. The video is available to download here at 59.94 frames per second, double the rate YouTube currently allows for UHD content. The music is titled \"Tides\" and is from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year6_HCblend_HD.png (1920x1080) [5.3 MB] || SDO_Year6_HCblend_HD.jpg (1920x1080) [545.9 KB] || SDO_Year6_HCblend_HD_print.jpg (1024x576) [179.5 KB] || SDO_Year6_HCblend_UHD.png (3840x2160) [19.7 MB] || SDO_Year6_HCblend_UHD.jpg (3840x2160) [1.2 MB] || SDO_Year6_HCblend_HD_searchweb.png (180x320) [59.6 KB] || SDO_Year6_HCblend_HD_thm.png (80x40) [4.8 KB] || 12144_SDO_Year_6_appletv.webm (1280x720) [50.5 MB] || 12144_SDO_Year_6_appletv.m4v (1280x720) [241.9 MB] || 12144_SDO_Year_6_appletv_appletv_subtitles.m4v (1280x720) [242.1 MB] || SDO_Year_6_SRT_Captions.en_US.srt [6.3 KB] || SDO_Year_6_SRT_Captions.en_US.vtt [6.3 KB] || 12144_SDO_Year_6_H264_Good_1920x1080_2997.mov (1920x1080) [1.4 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_2997.mov (3840x2160) [9.1 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_5994.mov (3840x2160) [10.2 GB] || 12144_SDO_Year_6_ProRes_3840x2160_5994.mov (3840x2160) [50.3 GB] || ", "hits": 109 }, { "id": 30726, "url": "https://svs.gsfc.nasa.gov/30726/", "result_type": "Hyperwall Visual", "release_date": "2015-11-19T09:00:00-05:00", "title": "NuSTAR Stares at the Sun", "description": "Blue-White areas in composite image with NuSTAR data show most energetic spots. || nustar_sun_PIA19821_print.jpg (1024x576) [80.4 KB] || nustar_sun_PIA19821_searchweb.png (180x320) [45.4 KB] || nustar_sun_PIA19821_thm.png (80x40) [9.5 KB] || nustar_sun_PIA19821.tif (5760x3240) [10.8 MB] || nustar_sun_30726.key [13.4 MB] || nustar_sun_30726.pptx [10.8 MB] || nustar_sun_PIA19821.hwshow [206 bytes] || ", "hits": 71 }, { "id": 11742, "url": "https://svs.gsfc.nasa.gov/11742/", "result_type": "Produced Video", "release_date": "2015-02-11T10:00:00-05:00", "title": "SDO: Year 5", "description": "Highlights from the Solar Dynamics Observatory's five years of watching the sun.The music is \"Expanding Universe\" and \"Facing the Unknown\" both from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.Information about the individual clips used in this video is here.Credit: NASA's Goddard Space Flight Center/SDO || Year_5_STILL_print.jpg (1024x576) [73.2 KB] || Year_5_STILL_1080.jpg (1920x1080) [289.2 KB] || Year_5_STILL_1080.png (1920x1080) [2.2 MB] || Year_5_STILL.png (3840x2160) [8.1 MB] || SDO_Year_5_List.jpg (2550x3300) [988.9 KB] || Year_5_STILL.jpg (3840x2160) [857.5 KB] || Year_5_STILL_web.jpg (320x180) [14.0 KB] || Year_5_STILL_searchweb.png (180x320) [31.7 KB] || Year_5_STILL_thm.png (80x40) [6.0 KB] || SDO-Year_5_Final_appletv.webm (960x540) [35.1 MB] || SDO-Year_5_Final_appletv_subtitles.m4v (960x540) [123.0 MB] || SDO-Year_5_Final_appletv.m4v (960x540) [123.2 MB] || SDO-Year_5_Final_1280x720.wmv (1280x720) [145.5 MB] || 11742_SDO-Year_5_MPEG4_1920X1080_2997.mp4 (1920x1080) [373.3 MB] || 11742_SDO-Year_5_H264_Good_1280x720_2997.mov (1280x720) [737.8 MB] || SDO-Year_5_Final_ipod_lg.m4v (640x360) [50.5 MB] || 11742_SDO-Year_5.en_US.vtt [1.3 KB] || 11742_SDO-Year_5.en_US.srt [1.3 KB] || 11742_SDO-Year_5_H264_Good_1920x1080_2997.mov (1920x1080) [1.6 GB] || SDO-Year_5_Final_ipod_sm.mp4 (320x240) [26.7 MB] || 11742_SDO-Year_5_ProRes_1920x1080_2997.mov (1920x1080) [4.0 GB] || 11742_SDO-Year_5_H264_Best_1920x1080_2997.mov (1920x1080) [5.1 GB] || 11742_SDO-Year_5_MPEG4_1920X1080_2997.hwshow [123 bytes] || ", "hits": 179 }, { "id": 11739, "url": "https://svs.gsfc.nasa.gov/11739/", "result_type": "Produced Video", "release_date": "2015-01-20T11:00:00-05:00", "title": "Telescope on NASA's SDO Collects Its 100 Millionth Image", "description": "100 million images of the sun: The Advanced Imaging Assembly on NASA's Solar Dynamics Observatory captured its 100 millionth image of the sun on Jan. 19, 2015. The image shows the glow in the solar atmosphere of gases at about 1.5 million Kelvin. Credit: NASA/SDO/AIA/LMSAL || SDO_AIA_193_100Millionth_print.jpg (1024x1024) [168.6 KB] || SDO_AIA_193_100Millionth.jpeg (4096x4096) [2.4 MB] || SDO_AIA_193_100Millionth_web.jpg (320x320) [27.3 KB] || SDO_AIA_193_100Millionth_searchweb.png (320x180) [95.6 KB] || SDO_AIA_193_100Millionth_thm.png (80x40) [10.2 KB] || ", "hits": 123 }, { "id": 11670, "url": "https://svs.gsfc.nasa.gov/11670/", "result_type": "Produced Video", "release_date": "2014-10-03T15:00:00-04:00", "title": "Sun Emits Mid-Level Flare on October 2, 2014", "description": "The sun emitted a mid-level solar flare, peaking at 3:01 p.m. EDT on Oct. 2, 2014. NASA's Solar Dynamics Observatory, which watches the sun 24-hours a day, captured images of the flare. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel.This flare is classified as an M7.3 flare. M-class flares are one-tenth as powerful as the most powerful flares, which are designated X-class flares. || ", "hits": 121 }, { "id": 11558, "url": "https://svs.gsfc.nasa.gov/11558/", "result_type": "Produced Video", "release_date": "2014-09-24T10:00:00-04:00", "title": "NASA's Many Views of a Massive CME", "description": "On July 23, 2012, a massive cloud of solar material erupted off the sun's right side, zooming out into space. It soon passed one of NASA's Solar Terrestrial Relations Observatory, or STEREO, spacecraft, which clocked the CME as traveling between 1,800 and 2,200 miles per second as it left the sun. This was the fastest CME ever observed by STEREO. Two other observatories – NASA's Solar Dynamics Observatory and the joint European Space Agency/NASA Solar and Heliospheric Observatory — witnessed the eruption as well. The July 2012 CME didn't move toward Earth, but watching an unusually strong CME like this gives scientists an opportunity to observe how these events originate and travel through space. STEREO's unique viewpoint from the sides of the sun combined with the other two observatories watching from closer to Earth helped scientists create models of the entire July 2012 event. They learned that an earlier, smaller CME helped clear the path for the larger event, thus contributing to its unusual speed. Such data helps advance our understanding of what causes CMEs and improves modeling of similar CMEs that could be Earth-directed. || ", "hits": 134 }, { "id": 11564, "url": "https://svs.gsfc.nasa.gov/11564/", "result_type": "Produced Video", "release_date": "2014-06-10T11:00:00-04:00", "title": "Sun Emits 3 X-class Flares in 2 Days", "description": "The sun emitted a significant solar flare, peaking at 7:42 a.m. EDT on June 10, 2014. NASA's Solar Dynamics Observatory – which typically observes the entire sun 24 hours a day — captured images of the flare. This flare is classified as an X2.2 flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc.About one hour later, the sun released a second X-class flare, peaking at 8:52 a.m. EDT on June 10, 2014. This is classified as an X1.5 flare. || ", "hits": 78 }, { "id": 11460, "url": "https://svs.gsfc.nasa.gov/11460/", "result_type": "Produced Video", "release_date": "2014-02-11T12:00:00-05:00", "title": "SDO: Year 4", "description": "The sun is always changing and NASA's Solar Dynamics Observatory is always watching. Launched on Feb. 11, 2010, SDO keeps a 24-hour eye on the entire disk of the sun, with a prime view of the graceful dance of solar material coursing through the sun's atmosphere, the corona. SDO's fourth year in orbit was no exception: NASA is releasing a movie of some of SDO's best sightings of the year, including massive solar explosions and giant sunspot shows. SDO captures images of the sun in 10 different wavelengths, each of which helps highlight a different temperature of solar material. Different temperatures can, in turn, show specific structures on the sun such as solar flares, which are giant explosions of light and x-rays, or coronal loops, which are streams of solar material traveling up and down looping magnetic field lines. The movie shows examples of both, as well as what's called prominence eruptions, when masses of solar material leap off the sun. The movie also shows a sunspot group on the solar surface. This sunspot, a magnetically strong and complex region appearing in mid-January 2014, was one of the largest in nine years. Scientists study these images to better understand the complex electromagnetic system causing the constant movement on the sun, which can ultimately have an effect closer to Earth, too: Flares and another type of solar explosion called coronal mass ejections can sometimes disrupt technology in space. Moreover, studying our closest star is one way of learning about other stars in the galaxy. NASA's Goddard Space Flight Center in Greenbelt, Md. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.SDO: Year One here.SDO: Year 2 here.SDO: Year 3 here.Information about the individual clips used in this video is here. || ", "hits": 107 }, { "id": 11387, "url": "https://svs.gsfc.nasa.gov/11387/", "result_type": "Produced Video", "release_date": "2013-10-29T16:30:00-04:00", "title": "Five Days of Flares and CMEs", "description": "This movie shows 23 of the 26 M- and X-class flares on the sun between 18:00 UT Oct. 23 and 15:00 UT Oct. 28, 2013, as captured by NASA's Solar Dynamics Observatory. It also shows the coronal mass ejections — great clouds of solar material bursting off the sun into space — during that time as captured by the ESA/NASA Solar and Heliospheric Observatory. || ", "hits": 94 }, { "id": 11379, "url": "https://svs.gsfc.nasa.gov/11379/", "result_type": "Produced Video", "release_date": "2013-10-24T10:00:00-04:00", "title": "Filament Eruption Creates 'Canyon of Fire' on the Sun", "description": "A magnetic filament of solar material erupted on the sun in late September, breaking the quiet conditions in a spectacular fashion. The 200,000 mile long filament ripped through the sun's atmosphere, the corona, leaving behind what looks like a canyon of fire. The glowing canyon traces the channel where magnetic fields held the filament aloft before the explosion. Visualizers at NASA's Goddard Space Flight Center in Greenbelt, Md. combined two days of satellite data to create a short movie of this gigantic event on the sun.In reality, the sun is not made of fire, but of something called plasma: particles so hot that their electrons have boiled off, creating a charged gas that is interwoven with magnetic fields. These images were captured on Sept. 29-30, 2013, by NASA's Solar Dynamics Observatory, or SDO, which constantly observes the sun in a variety of wavelengths. Different wavelengths help capture different aspect of events in the corona. The red images shown in the movie help highlight plasma at temperatures of 90,000° F and are good for observing filaments as they form and erupt. The yellow images, showing temperatures at 1,000,000° F, are useful for observing material coursing along the sun's magnetic field lines, seen in the movie as an arcade of loops across the area of the eruption. The browner images at the beginning of the movie show material at temperatures of 1,800,000° F, and it is here where the canyon of fire imagery is most obvious. By comparing this with the other colors, one sees that the two swirling ribbons moving farther away from each other are, in fact, the footprints of the giant magnetic field loops, which are growing and expanding as the filament pulls them upward. || ", "hits": 216 }, { "id": 10785, "url": "https://svs.gsfc.nasa.gov/10785/", "result_type": "Produced Video", "release_date": "2013-05-07T11:00:00-04:00", "title": "NASA's Heliophysics Fleet Captures May 1, 2013 Prominence Eruption and CME", "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region just around the East limb (left edge) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 angstroms, SDO provided a beautiful view of the initial arc as it left the solar surface. Such eruptions soon leave SDO's field of view, but other satellites in NASA's Heliophysics fleet can pick them up, tracking such space weather to determine if they are headed toward Earth or spacecraft near other planets. With advance warning, many space assets can be put into safe mode and protect themselves from the effects of such particle radiation.In addition to the images captured by SDO, the May 1, 2013 CME was also observed by the ESA/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping coronagraphs—telescopes where the bright sun is blocked by a disk so it doesn't overpower the fainter solar atmosphere—and they both saw the CME continue outward. The LASCO C2 coronagraph shows the region out to about 2.5 million miles. The LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun.NASA's Solar Terrestrial Relations Observatory (STEREO) Ahead satellite saw the eruption from a very different angle. It, along with its twin STEREO Behind, is orbiting at a similar distance as Earth. STEREO-A orbits slightly faster than Earth and STEREO-B orbits slightly slower. Currently, STEREO-A is more than two-thirds of the way to being directly behind the sun, and has a view of the far side of the sun. From this perspective, the CME came off the right side of the sun. STEREO has an extreme ultraviolet camera similar to SDO's, but it also has coronagraphs like SOHO. As a result, using its two inner coronagraphs, it was able to track the CME from the solar surface out to 6.3 million miles.Working together, such missions provide excellent coverage of a wide variety of solar events, a wealth of scientific data—and lots of beautiful imagery.Watch this video on YouTube. || ", "hits": 100 }, { "id": 11262, "url": "https://svs.gsfc.nasa.gov/11262/", "result_type": "Produced Video", "release_date": "2013-05-03T21:30:00-04:00", "title": "Sun Emits Mid-Level Flare and Prominence Eruption", "description": "The sun emitted a mid-level solar flare, peaking at 1:32 pm EDT on May 3, 2013. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel. This disrupts the radio signals for as long as the flare is ongoing, and the radio blackout for this flare has already subsided.This flare is classified as an M5.7-class flare. M-class flares are the weakest flares that can still cause some space weather effects near Earth. Increased numbers of flares are quite common at the moment, as the sun's normal 11-year activity cycle is ramping up toward solar maximum, which is expected in late 2013. || ", "hits": 149 }, { "id": 11255, "url": "https://svs.gsfc.nasa.gov/11255/", "result_type": "Produced Video", "release_date": "2013-04-22T14:00:00-04:00", "title": "Three Years of SDO Images", "description": "In the three years since it first provided images of the sun in the spring of 2010, NASA's Solar Dynamics Observatory (SDO) has had virtually unbroken coverage of the sun's rise toward solar maximum, the peak of solar activity in its regular 11-year cycle. This video shows those three years of the sun at a pace of two images per day. Each image is displayed for two frames at a 29.97 frame rate.SDO's Atmospheric Imaging Assembly (AIA) captures a shot of the sun every 12 seconds in 10 different wavelengths. The images shown here are based on a wavelength of 171 angstroms, which is in the extreme ultraviolet range and shows solar material at around 600,000 Kelvin. In this wavelength it is easy to see the sun's 25-day rotation as well as how solar activity has increased over three years.During the course of the video, the sun subtly increases and decreases in apparent size. This is because the distance between the SDO spacecraft and the sun varies over time. The image is, however, remarkably consistent and stable despite the fact that SDO orbits the Earth at 6,876 miles per hour and the Earth orbits the sun at 67,062 miles per hour.Such stability is crucial for scientists, who use SDO to learn more about our closest star. These images have regularly caught solar flares and coronal mass ejections in the act, types of space weather that can send radiation and solar material toward Earth and interfere with satellites in space. SDO's glimpses into the violent dance on the sun help scientists understand what causes these giant explosions — with the hopes of some day improving our ability to predict this space weather.The four wavelength view at the end of the video shows light at 4500 angstroms, which is basically the visible light view of the sun, and reveals sunspots; light at 193 angstroms which highlights material at 1 million Kelvin and reveals more of the sun's corona; light at 304 angstroms which highlights material at around 50,000 Kelvin and shows features in the transition region and chromosphere of the sun; and light at 171 angstroms.Noteworthy events that appear briefly in the main sequence of this video:00:30;24 Partial eclipse by the moon00:31;16 Roll maneuver01:11;02 August 9, 2011 X6.9 Flare, currently the largest of this solar cycle01:28;07 Comet Lovejoy, December 15, 201101:42;29 Roll Maneuver01:51;07 Transit of Venus, June 5, 201202:28;13 Partial eclipse by the moonWatch this video on YouTube. || ", "hits": 207 }, { "id": 11246, "url": "https://svs.gsfc.nasa.gov/11246/", "result_type": "Produced Video", "release_date": "2013-04-11T12:00:00-04:00", "title": "The Sun Emits a Mid-level Flare and CME", "description": "The sun emitted a mid-level flare, peaking at 3:16 a.m. EDT on April 11, 2013.Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel. This disrupts the radio signals for as long as the flare is ongoing, anywhere from minutes to hours.This flare is classified as an M6.5 flare, some ten times less powerful than the strongest flares, which are labeled X-class flares. M-class flares are the weakest flares that can still cause some space weather effects near Earth. This flare produced a radio blackout that has since subsided. The blackout was categorized as an R2 on a scale between R1 and R5 on NOAA's space weather scales.This is the strongest flare seen so far in 2013. Increased numbers of flares are quite common at the moment, since the sun's normal 11-year activity cycle is ramping up toward solar maximum, which is expected in late 2013. Humans have tracked this solar cycle continuously since it was discovered, and it is normal for there to be many flares a day during the sun's peak activity. || ", "hits": 86 }, { "id": 11211, "url": "https://svs.gsfc.nasa.gov/11211/", "result_type": "Produced Video", "release_date": "2013-02-22T10:00:00-05:00", "title": "SDO Observes Fast-Growing Sunspot", "description": "As magnetic fields on the sun rearrange and realign, dark spots known as sunspots can appear on its surface. Over the course of Feb. 19-20, 2013, scientists watched a giant sunspot form in under 48 hours. It has grown to over six Earth diameters across but its full extent is hard to judge since the spot lies on a sphere not a flat disk.The spot quickly evolved into what's called a delta region, in which the lighter areas around the sunspot, the penumbra, exhibit magnetic fields that point in the opposite direction of those fields in the center, dark area. This is a fairly unstable configuration that scientists know can lead to eruptions of radiation on the sun called solar flares. || ", "hits": 119 }, { "id": 11168, "url": "https://svs.gsfc.nasa.gov/11168/", "result_type": "Produced Video", "release_date": "2013-02-20T10:00:00-05:00", "title": "SDO Sees Fiery Looping Rain on the Sun", "description": "Eruptive events on the sun can be wildly different. Some come just with a solar flare, some with an additional ejection of solar material called a coronal mass ejection (CME), and some with complex moving structures in association with changes in magnetic field lines that loop up into the sun's atmosphere, the corona. On July 19, 2012, an eruption occurred on the sun that produced all three. A moderately powerful solar flare exploded on the sun's lower right hand limb, sending out light and radiation. Next came a CME, which shot off to the right out into space. And then, the sun treated viewers to one of its dazzling magnetic displays — a phenomenon known as coronal rain. Over the course of the next day, hot plasma in the corona cooled and condensed along strong magnetic fields in the region. Magnetic fields, themselves, are invisible, but the charged plasma is forced to move along the lines, showing up brightly in the extreme ultraviolet wavelength of 304 angstroms, which highlights material at a temperature of about 50,000 Kelvin. This plasma acts as a tracer, helping scientists watch the dance of magnetic fields on the sun, outlining the fields as it slowly falls back to the solar surface. The footage in this video was collected by the Solar Dynamics Observatory's AIA instrument. SDO collected one frame every 12 seconds, and the movie plays at 30 frames per second, so each second in this video corresponds to 6 minutes of real time. The video covers 12:30 a.m. EDT to 10:00 p.m. EDT on July 19, 2012.Watch this video on YouTube. || ", "hits": 187 }, { "id": 11203, "url": "https://svs.gsfc.nasa.gov/11203/", "result_type": "Produced Video", "release_date": "2013-02-11T10:00:00-05:00", "title": "SDO: Year 3", "description": "On Feb. 11, 2010, NASA launched an unprecedented solar observatory into space. The Solar Dynamics Observatory (SDO) flew up on an Atlas V rocket, carrying instruments that scientists hoped would revolutionize observations of the sun. If all went according to plan, SDO would provide incredibly high-resolution data of the entire solar disk almost as quickly as once a second. When the science team released its first images in April of 2010, SDO's data exceeded everyone's hopes and expectations, providing stunningly detailed views of the sun. In the three years since then, SDO's images have continued to show breathtaking pictures and movies of eruptive events on the sun. Such imagery is more than just pretty, they are the very data that scientists study. By highlighting different wavelengths of light, scientists can track how material on the sun moves. Such movement, in turn, holds clues as to what causes these giant explosions, which, when Earth-directed, can disrupt technology in space. SDO is the first mission in a NASA's Living With a Star program, the goal of which is to develop the scientific understanding necessary to address those aspects of the sun-Earth system that directly affect our lives and society. NASA's Goddard Space Flight Center in Greenbelt, Md. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.SDO: Year One here.SDO: Year 2 here.Information about the individual clips used in this video is here.Watch this video on YouTube. || ", "hits": 82 }, { "id": 11207, "url": "https://svs.gsfc.nasa.gov/11207/", "result_type": "Produced Video", "release_date": "2013-02-07T10:30:00-05:00", "title": "The Sun Produces Two CMEs", "description": "In the evening of Feb. 5, 2013, the sun erupted with two coronal mass ejections or CMEs that may glance near-Earth space. Experimental NASA research models, based on observations from the Solar Terrestrial Relations Observatory (STEREO) and ESA/NASA's Solar and Heliospheric Observatory, show that the first CME began at 7 p.m. EST and left the sun at speeds of around 750 miles per second. The second CME began at 10:36 p.m. EST and left the sun at speeds of around 350 miles per second. Historically, CMEs of this speed and direction have been benign.Not to be confused with a solar flare, a CME is a solar phenomenon that can send solar particles into space and reach Earth one to three days later.Earth-directed CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they connect with the outside of the Earth's magnetic envelope, the magnetosphere, for an extended period of time. In the past, CMEs at this strength have had little effect. They may cause auroras near the poles but are unlikely to disrupt electrical systems on Earth or interfere with GPS or satellite-based communications systems. || ", "hits": 74 }, { "id": 11180, "url": "https://svs.gsfc.nasa.gov/11180/", "result_type": "Produced Video", "release_date": "2013-01-31T13:00:00-05:00", "title": "SDO Provides First Sightings of How
a CME Forms", "description": "On July 18, 2012, a fairly small explosion of light burst off the lower right limb of the sun. Such flares often come with an associated eruption of solar material, known as a coronal mass ejection or CME — but this one did not. Something interesting did happen, however. Magnetic field lines in this area of the sun's atmosphere, the corona, began to twist and kink, generating the hottest solar material — a charged gas called plasma — to trace out the newly-formed slinky shape. The plasma glowed brightly in extreme ultraviolet images from the Atmospheric Imaging Assembly (AIA) aboard NASA's Solar Dynamics Observatory (SDO) and scientists were able to watch for the first time the very formation of something they had long theorized was at the heart of many eruptive events on the sun: a flux rope. Eight hours later, on July 19, the same region flared again. This time the flux rope's connection to the sun was severed, and the magnetic fields escaped into space, dragging billions of tons of solar material along for the ride — a classic CME. More than just gorgeous to see, such direct observation offers one case study on how this crucial kernel at the heart of a CME forms. Such flux ropes have been seen in images of CMEs as they fly away from the sun, but it's never been known — indeed, has been strongly debated — whether the flux rope formed before or in conjunction with a CME's launch. This case shows a clear-cut example of the flux rope forming ahead of time.Watch this video on YouTube. || ", "hits": 113 }, { "id": 11201, "url": "https://svs.gsfc.nasa.gov/11201/", "result_type": "Produced Video", "release_date": "2013-01-31T12:00:00-05:00", "title": "January 31, 2013 CME and Prominence Eruption", "description": "On Jan. 31, 2013 at 2:09am EST, the sun erupted with an Earth-directed coronal mass ejection or CME. Experimental NASA research models, based on observations from the Solar Terrestrial Relations Observatory (STEREO) and ESA/NASA's Solar and Heliospheric Observatory, show that the CME left the sun at speeds of around 575 miles per second, which is a fairly typical speed for CMEs. Historically, CMEs at this speed are mild.Not to be confused with a solar flare, a CME is a solar phenomenon that can send solar particles into space and reach Earth one to three days later.Earth-directed CMEs can cause a space weather phenomenon called a geomagnetic storm, which occurs when they connect with the outside of the Earth's magnetic envelope, the magnetosphere, for an extended period of time. In the past, CME's such as this have caused auroras near the poles but didn't disrupt electrical systems on Earth or interfere with GPS or satellite-based communications systems. || ", "hits": 68 }, { "id": 11071, "url": "https://svs.gsfc.nasa.gov/11071/", "result_type": "Produced Video", "release_date": "2013-01-23T11:30:00-05:00", "title": "SDO Wavelength Graphics", "description": "Specialized instruments, either in ground-based or space-based telescopes, can observe light far beyond the ranges visible to the naked eye. Different wavelengths convey information about different components of the sun's surface and atmosphere, so scientists use them to paint a full picture of our constantly changing and varying star.Yellow light of 5800 angstroms, for example, generally emanates from material of about 10,000 degrees F (5700 degrees C), which represents the surface of the sun. Extreme ultraviolet light of 94 angstroms, on the other hand, comes from atoms that are about 11 million degrees F (6,300,000 degrees C) and is a good wavelength for looking at solar flares, which can reach such high temperatures. By examining pictures of the sun in a variety of wavelengths — as is done through such telescopes as NASA's Solar Dynamics Observatory (SDO), NASA's Solar Terrestrial Relations Observatory (STEREO) and the ESA/NASA Solar and Heliospheric Observatory (SOHO) — scientists can track how particles and heat move through the sun's atmosphere.We see the visible spectrum of light simply because the sun is made up of a hot gas — heat produces light just as it does in an incandescent light bulb. But when it comes to the shorter wavelengths, the sun sends out extreme ultraviolet light and x-rays because it is filled with many kinds of atoms, each of which give off light of a certain wavelength when they reach a certain temperature. Not only does the sun contain many different atoms — helium, hydrogen, iron, for example — but also different kinds of each atom with different electrical charges, known as ions. Each ion can emit light at specific wavelengths when it reaches a particular temperature. Scientists have cataloged which atoms produce which wavelengths since the early 1900s, and the associations are well documented in lists that can take up hundreds of pages.Instruments that produce conventional images of the sun focus exclusively on light around one particular wavelength, sometimes not one that is visible to the naked eye. SDO scientists, for example, chose 10 different wavelengths to observe for its Atmospheric Imaging Assembly (AIA) instrument. Each wavelength is largely based on a single, or perhaps two types of ions — though slightly longer and shorter wavelengths produced by other ions are also invariably part of the picture. Each wavelength was chosen to highlight a particular part of the sun's atmosphere.From the sun's surface on out, the wavelengths SDO observes, measured in angstroms, are: 4500: Showing the sun's surface or photosphere. 1700: Shows surface of the sun, as well as a layer of the sun's atmosphere called the chromosphere, which lies just above the photosphere and is where the temperature begins rising. 1600: Shows a mixture between the upper photosphere and what's called the transition region, a region between the chromosphere and the upper most layer of the sun's atmosphere called the corona. The transition region is where the temperature rapidly rises. 304: This light is emitted from the chromosphere and transition region. 171: This wavelength shows the sun's atmosphere, or corona, when it's quiet. It also shows giant magnetic arcs known as coronal loops. 193: Shows a slightly hotter region of the corona, and also the much hotter material of a solar flare. 211: This wavelength shows hotter, magnetically active regions in the sun's corona. 335: This wavelength also shows hotter, magnetically active regions in the corona. 94: This highlights regions of the corona during a solar flare. 131: The hottest material in a flare. || ", "hits": 392 }, { "id": 11072, "url": "https://svs.gsfc.nasa.gov/11072/", "result_type": "Produced Video", "release_date": "2012-11-26T10:00:00-05:00", "title": "SDO Solar Comparison October 2010 to October 2012", "description": "The sun goes through a natural solar cycle approximately every 11 years. The cycle is marked by the increase and decrease of sunspots — visible as dark blemishes on the sun's surface, or photosphere. The greatest number of sunspots in any given solar cycle is designated as \"solar maximum.\" The lowest number is \"solar minimum.\" The solar cycle provides more than just increased sunspots, however. In the sun's atmosphere, or corona, bright active regions appear, which are rooted in the lower sunspots. Scientists track the active regions since they are often the origin of eruptions on the sun such as solar flares or coronal mass ejections. The most recent solar minimum occurred in 2008, and the sun began to ramp up in January 2010, with an M-class flare (a flare that is 10 times less powerful than the largest flares, labeled X-class). The sun has continued to get more active, with the next solar maximum predicted for 2013. The journey toward solar maximum is evident in current images of the sun, showing a marked difference from those of 2010, with bright active regions dotted around the star. || ", "hits": 65 }, { "id": 11111, "url": "https://svs.gsfc.nasa.gov/11111/", "result_type": "Produced Video", "release_date": "2012-10-05T10:00:00-04:00", "title": "Getting NASA's SDO into Focus", "description": "From Sep. 6 to Sep. 29, 2012, NASA's Solar Dynamic Observatory (SDO) moved into its semi-annual eclipse season, a time when Earth blocks the telescope's view of the sun for a period of time each day. Scientists choose orbits for solar telescopes to minimize eclipses as much as possible, but they are a fact of life — one that comes with a period of fuzzy imagery directly after the eclipse. The Helioseismic and Magnetic Imager (HMI) on SDO observes the sun through a glass window. The window can change shape in response to temperature changes, and does so dramatically and quickly when it doesn't directly feel the sun's heat. \"You've got a piece of glass looking at the sun, and then suddenly it isn't,\" says Dean Pesnell, the project scientist for SDO at NASA's Goddard Space Flight Center in Greenbelt, Md. \"The glass gets colder and flexes. It becomes like a lens. It's as if we put a set of eye glasses in front of the instrument, causing the observations to blur.\" To counteract this effect, HMI was built with heaters to warm the window during an eclipse. By adjusting the timing and temperature of the heater, the HMI team has learned the best procedures for improving resolution quickly. Without adjusting the HMI front window heaters, it takes about two hours to return to optimal observing. Over the two years since SDO launched in 2010, the team has brought the time it takes to get a clear image down from 60 minutes to around 45 to 50 minutes after an eclipse. \"We allocated an hour for these more blurry images,\" says Pesnell. \"And we've learned to do a lot better than that. With 45 eclipses a year, the team gets a lot of practice.\" SDO will enter its next eclipse season on March 3, 2013. || ", "hits": 63 }, { "id": 11046, "url": "https://svs.gsfc.nasa.gov/11046/", "result_type": "Produced Video", "release_date": "2012-07-19T10:00:00-04:00", "title": "Van Gogh Sun", "description": "A crucial, and often underappreciated, facet of science lies in deciding how to turn the raw numbers of data into useful, understandable information — often through graphs and images. Such visualization techniques are needed for everything from making a map of planetary orbits based on nightly measurements of where they are in the sky to colorizing normally invisible light such as X-rays to produce \"images\" of the sun.More information, of course, requires more complex visualizations and occasionally such images are not just informative, but beautiful too.Such is the case with a new technique created by Nicholeen Viall, a solar scientist at NASA's Goddard Space Flight Center in Greenbelt, Md. She creates images of the sun reminiscent of Van Gogh, with broad strokes of bright color splashed across a yellow background. But it's science, not art. The color of each pixel contains a wealth of information about the 12-hour history of cooling and heating at that particular spot on the sun. That heat history holds clues to the mechanisms that drive the temperature and movements of the sun's atmosphere, or corona.To look at the corona from a fresh perspective, Viall created a new kind of picture, making use of the high resolution provided by NASA's Solar Dynamics Observatory (SDO). SDO's Atmospheric Imaging Assembly (AIA) provides images of the sun in 10 different wavelengths, each approximately corresponding to a single temperature of material. Therefore, when one looks at the wavelength of 171 angstroms, for example, one sees all the material in the sun's atmosphere that is a million degrees Kelvin. By looking at an area of the sun in different wavelengths, one can get a sense of how different swaths of material change temperature. If an area seems bright in a wavelength that shows a hotter temperature an hour before it becomes bright in a wavelength that shows a cooler temperature, one can gather information about how that region has changed over time.Viall's images show a wealth of reds, oranges, and yellow, meaning that over a 12-hour period the material appear to be cooling. Obviously there must have been heating in the process as well, since the corona isn't on a one-way temperature slide down to zero degrees. Any kind of steady heating throughout the corona would have shown up in Viall's images, so she concludes that the heating must be quick and impulsive — so fast that it doesn't show up in her images. This lends credence to those theories that say numerous nanobursts of energy help heat the corona. || ", "hits": 43 }, { "id": 10996, "url": "https://svs.gsfc.nasa.gov/10996/", "result_type": "Produced Video", "release_date": "2012-06-05T00:00:00-04:00", "title": "SDO's Ultra-high Definition View of 2012 Venus Transit", "description": "Launched on Feb. 11, 2010, the Solar Dynamics Observatory, or SDO, is the most advanced spacecraft ever designed to study the sun. During its five-year mission, it will examine the sun's atmosphere, magnetic field and also provide a better understanding of the role the sun plays in Earth's atmospheric chemistry and climate. SDO provides images with resolution 8 times better than high-definition television and returns more than a terabyte of data each day.On June 5 2012, SDO collected images of the rarest predictable solar event—the transit of Venus across the face of the sun. This event lasted approximately 6 hours and happens in pairs eight years apart, which are separated from each other by 105 or 121 years. The last transit was in 2004 and the next will not happen until 2117.The videos and images displayed here are constructed from several wavelengths of extreme ultraviolet light and a portion of the visible spectrum. The red colored sun is the 304 angstrom ultraviolet, the golden colored sun is 171 angstrom, the magenta sun is 1700 angstrom, and the orange sun is filtered visible light. 304 and 171 show the atmosphere of the sun, which does not appear in the visible part of the spectrum. || ", "hits": 852 }, { "id": 10990, "url": "https://svs.gsfc.nasa.gov/10990/", "result_type": "Produced Video", "release_date": "2012-05-23T14:00:00-04:00", "title": "Incandescent Sun", "description": "This video takes SDO images and applies additional processing to enhance the structures visible. While there is no scientific value to this processing, it does result in a beautiful, new way of looking at the sun. The original frames are in the 171 angstrom wavelength of extreme ultraviolet. This wavelength shows plasma in the solar atmosphere, called the corona, that is around 600,000 Kelvin. The loops represent plasma held in place by magnetic fields. They are concentrated in \"active regions\" where the magnetic fields are the strongest. These active regions usually appear in visible light as sunspots. The events in this video represent 24 hours of activity on September 25, 2011. || ", "hits": 54 }, { "id": 10962, "url": "https://svs.gsfc.nasa.gov/10962/", "result_type": "Produced Video", "release_date": "2012-04-16T17:00:00-04:00", "title": "Big Blast—April 16th Flare and CME", "description": "A beautiful prominence eruption producing a coronal mass ejection (CME) shot off the east limb (left side) of the sun on April 16, 2012. Such eruptions are often associated with solar flares, and in this case an M1 class (medium-sized) flare occurred at the same time, peaking at 1:45 PM EDT. The CME was not aimed toward Earth.For full 4k frames of the April 15 small eruption and April 16 large eruption go here. || ", "hits": 76 }, { "id": 10957, "url": "https://svs.gsfc.nasa.gov/10957/", "result_type": "Produced Video", "release_date": "2012-03-05T00:00:00-05:00", "title": "New Active Region on Sun Produces Three Flares Including an X1 on March 5", "description": "On March 2, 2012 a new active region on the sun, region 1429, rotated into view. It has let loose two M-class flares and one X-class so far. The M-class flares erupted on March 2 and on March 4. The third flare, rated an X1, peaked at 10:30 ET on March 4. A CME accompanied each flare, though due to the fact that this active region is still off to the side of the sun, they will likely have a weak effect on Earth's magnetosphere.The M class flare on March 4 flare also came with what's called a Type IV radio burst that lasted for about 46 minutes. Sending out broadband radio waves, these bursts can occur towards the end of a solar flare and are believed to be created by moving electrons trapped in great, looping magnetic fields left over from the initial flare. The bursts can interfere with radio communications on Earth. || ", "hits": 45 }, { "id": 10886, "url": "https://svs.gsfc.nasa.gov/10886/", "result_type": "Produced Video", "release_date": "2011-12-19T22:00:00-05:00", "title": "SDO Sees Comet Lovejoy Survive Close Encounter With Sun", "description": "One instrument watching for the comet was the Solar Dynamics Observatory (SDO), which adjusted its cameras in order to watch the trajectory. Not only does this help with comet research, but it also helps orient instruments on SDO—since the scientists know where the comet is based on other spacecraft, they can finely determine the position of SDO's mirrors. This first clip from SDO from the evening of Dec 15, 2011 shows Comet Lovejoy moving in toward the sun. Comet Lovejoy survived its encounter with the sun. The second clip shows the comet exiting from behind the right side of the sun, after an hour of travel through its closest approach to the sun. By tracking how the comet interacts with the sun's atmosphere, the corona, and how material from the tail moves along the sun's magnetic field lines, solar scientists hope to learn more about the corona. This movie was filmed by the Solar Dynamics Observatory in 171 angstrom wavelength, which is typically shown in yellow.Credit: NASA/SDO || ", "hits": 69 }, { "id": 10817, "url": "https://svs.gsfc.nasa.gov/10817/", "result_type": "Produced Video", "release_date": "2011-09-07T12:00:00-04:00", "title": "SDO EVE Late Phase Flares", "description": "Scientists have been seeing just the tip of the iceberg when monitoring flares with X-rays. With the complete extreme ultraviolet (EUV) coverage by the SDO EUV Variability Experiment (EVE), they have observed enhanced EUV radiation that appears not only during the X-ray flare, but also a second time delayed by many minutes after the X-ray flare peak. These delayed, second peaks are referred to as the EUV Late Phase contribution to flares.The solar EUV radiation creates our Earth's ionosphere (plasma in our atmosphere), so solar flares disturb our ionosphere and consequently our communication and navigation technologies, such as Global Positioning System (GPS), that transmit through the ionosphere. For over 30 years, scientists have relied on the GOES X-ray monitor to tell them when to expect disturbances to our ionosphere. With these new SDO EVE results, they now recognize that additional ionospheric disturbances from these later EUV enhancements are also a concern. || ", "hits": 68 }, { "id": 10551, "url": "https://svs.gsfc.nasa.gov/10551/", "result_type": "Produced Video", "release_date": "2010-06-10T00:00:00-04:00", "title": "SDO First Light Press Conference", "description": "A unique NASA spacecraft launched February 11, 2010, called the Solar Dynamics Observatory, or SDO, has started delivering images of the sun that have astonished scientists. SDO is the most advanced spacecraft ever designed to study the sun and its dynamic behavior. The spacecraft can produce images with clarity ten times better than high definition television and provide more comprehensive science data faster than any solar observing spacecraft in history. The goal of the mission is to help scientists study solar activity to improve forecasts of how the sun affects Earth.On April 21, 2010, NASA held a live press conference at the Newseum in Washington D.C. to unveil the first images and videos from SDO—SDO's First Light.A version of the press conference with captioning is available. || ", "hits": 44 }, { "id": 10538, "url": "https://svs.gsfc.nasa.gov/10538/", "result_type": "Produced Video", "release_date": "2009-12-04T00:00:00-05:00", "title": "SDO Beauty Pass", "description": "Solar Dynamic Observatory in orbit around the Earth || Solar Dynamic Observatory in orbit around the Earth || SDO_shotOne0747.00877_print.jpg (1024x576) [52.1 KB] || SDO_shotOne0747_web.png (320x180) [242.5 KB] || SDO_shotOne0747_thm.png (80x40) [14.9 KB] || bo.webmhd.webm (960x540) [10.7 MB] || 1280x720_16x9_60p (1280x720) [256.0 KB] || bo.mp4 (1280x720) [9.0 MB] || ", "hits": 40 }, { "id": 10539, "url": "https://svs.gsfc.nasa.gov/10539/", "result_type": "Produced Video", "release_date": "2009-12-04T00:00:00-05:00", "title": "SDO in Orbit", "description": "This animation show the Solar Dynamics Observatory in orbit around Earth || SDO in orbit || SDO_BPTWO0368.00377_print.jpg (1024x576) [59.6 KB] || SDO_BPTWO0368_web.png (320x180) [282.2 KB] || SDO_BPTWO0368_thm.png (80x40) [15.8 KB] || SDO_orbit_720p.webmhd.webm (960x540) [3.4 MB] || 1280x720_16x9_60p (1280x720) [0 Item(s)] || SDO_orbit_720p.m2v (1280x720) [27.1 MB] || orbit.mp4 (1280x720) [3.5 MB] || SDO_orbit_512x288.m1v (512x288) [4.3 MB] || ", "hits": 68 }, { "id": 10261, "url": "https://svs.gsfc.nasa.gov/10261/", "result_type": "Produced Video", "release_date": "2008-07-02T15:00:00-04:00", "title": "Hello, SDO", "description": "Meet Little SDO! This animated version of NASA's Solar Dynamics Observatory is here to introduce you to all the great new ways we'll be looking at the sun and predicting how it will affect our lives on Earth. || ", "hits": 26 }, { "id": 10199, "url": "https://svs.gsfc.nasa.gov/10199/", "result_type": "Produced Video", "release_date": "2008-04-03T00:00:00-04:00", "title": "SDO Solar Array and High Gain Antenna Test Deploy", "description": "Goddard engineers attached the solar array panels and high gain antennas to the Solar Dynamics Observatory. During launch the arrays and antennas are tucked in against the spacecraft and must be opened up for use on orbit. This video show the engineers testing that deployment. The arrays and antennas are held against the spacecraft by explosive bolts that are exploded to allow them to open. The same type of explosives will deploy the solar arrays in space. The solar arrays will collect energy from the Sun to power the spacecraft. SDO will collect so much data on the sun that it could not be stored on the spacecraft and therefore must be sent to the ground quickly. The high gain antennas will transmit 1.5 terabytes of data each day to a ground station at White Sands, NM. That's like watching 380 movies each day! || ", "hits": 33 }, { "id": 10189, "url": "https://svs.gsfc.nasa.gov/10189/", "result_type": "Produced Video", "release_date": "2008-03-11T00:00:00-04:00", "title": "Stepping Stones to SDO", "description": "NASA's Solar Dynamics Observatory (SDO) is currently in the 'integration and test' phase of mission development, (i.e. observatory is now complete with the spacecraft bus, propulsion module and instruments), the ground system is being completed and flight software is being tested. Critical systems testing has already begun and environmental testing of he observatory will be conducted in the near future as they continue towards a launch readiness date of December 1, 2008. This series of short videos shows the SDO spacecraft being assembled and tested with narration by the engineers doing the work. It will be updated until SDO is ready for launch.For more information on SDO, visit the web site http://sdo.gsfc.nasa.gov || ", "hits": 43 }, { "id": 10188, "url": "https://svs.gsfc.nasa.gov/10188/", "result_type": "Produced Video", "release_date": "2008-03-02T00:00:00-05:00", "title": "NASA's SDO Mission", "description": "A new NASA spacecraft called the Solar Dynamics Observatory (SDO) will deliver startling images of the sun with ten times more detail than HDTV. The goal of the mission is to help scientists zoom in on solar activity such as sunspots, solar flares and coronal mass ejections, thus improving forcasts of solar storms. The complete script is available. For more information on the Solar Dynamics Observatory, check out their web site at http://sdo.gsfc.nasa.gov. || ", "hits": 62 }, { "id": 10190, "url": "https://svs.gsfc.nasa.gov/10190/", "result_type": "Produced Video", "release_date": "2008-02-26T00:00:00-05:00", "title": "SDO: Command Accepted!", "description": "Music Video - NASA's Solar Dyamics Observatory (SDO) will help scientists to better understand solar variability and aid in predictions of space weather. The new Ka band antennas at the White Sands Testing Facility in New Mexico will be the go-between the satellite and the SDO Mission Operations Contol Center. || ", "hits": 29 }, { "id": 20118, "url": "https://svs.gsfc.nasa.gov/20118/", "result_type": "Animation", "release_date": "2007-09-10T00:00:00-04:00", "title": "The Solar Dynamics Observatory (SDO)", "description": "SDO is designed to help us understand the Sun's influence on Earth and Near-Earth space by studying the solar atmosphere on small scales of space and time and in many wavelengths simultaneously. || ", "hits": 605 }, { "id": 3435, "url": "https://svs.gsfc.nasa.gov/3435/", "result_type": "Visualization", "release_date": "2007-08-14T00:00:00-04:00", "title": "Solar Dynamics Observatory (SDO): Data Collection Comparison", "description": "Solar Dynamics Observatory (SDO) will dramatically increase our ability to collect data about the Sun. This visualization compares the temporal and spatial resolution of SOHO/EIT with TRACE. SDO will enable TRACE-like image and temporal resolution over the entire solar disk. This movie opens with a full-disk view of the Sun in ultraviolet light (195 angstroms) from SOHO/EIT using the traditional TRACE 'gold' color table. We zoom in on the active region on the western limb where the TRACE instrument is pointing and fade-in an inset of the higher-resolution TRACE data. To emphasize the comparison, the TRACE inset is moved aside (with a solid white border) revealing the matching EIT data view (enclosed in the faint white border). At this point, we step through the time series of data frames. In this movie, much of the TRACE imagery is collected at time intervals between 3 and 40 seconds. On the other hand, a new SOHO/EIT image is taken about every 12 minutes (720 seconds). The SDO Atmospheric Imaging Assembly (AIA) will take full-disk solar images at four times the SOHO/EIT spatial resolution, a whopping 4096x4096, and at least 70 times the temporal resolution, 10 seconds or better per image. This creates a data rate over 1000x higher than SOHO/EIT. It is roughly equivalent to TRACE spatial and temporal resolution, but over the entire solar disk. || ", "hits": 64 }, { "id": 20038, "url": "https://svs.gsfc.nasa.gov/20038/", "result_type": "Animation", "release_date": "2004-12-03T12:00:00-05:00", "title": "Solar Dynamics Observatory On-Station", "description": "Animation of the Solar Dynamics Observatory (SDO) in it's deployed location. || 'Beauty Pass' of Solar Dynamics Observatory on-station. || SDO_pre.00002_print.jpg (1024x691) [86.7 KB] || SDO_thm.png (80x40) [16.5 KB] || SDO_pre.jpg (320x197) [8.3 KB] || SDOSml_pre.jpg (320x219) [9.6 KB] || SDOSml_pre_searchweb.jpg (320x180) [73.5 KB] || SDO.webmhd.webm (960x540) [6.7 MB] || SDO.mpg (720x486) [4.3 MB] || SDOSml.mpg (320x240) [4.3 MB] || ", "hits": 131 } ] }