{ "count": 38, "next": null, "previous": null, "results": [ { "id": 31381, "url": "https://svs.gsfc.nasa.gov/31381/", "result_type": "Hyperwall Visual", "release_date": "2026-03-31T11:51:59-04:00", "title": "NASA’S PUNCH Images Eruptions from the Sun", "description": "This video shows several coronal mass ejections (CMEs) erupting from the Sun’s surface from Oct. 21 to Nov. 12, 2025.", "hits": 1251 }, { "id": 40548, "url": "https://svs.gsfc.nasa.gov/gallery/solarand-heliospheric-observatory-soho/", "result_type": "Gallery", "release_date": "2026-03-03T00:00:00-05:00", "title": "SOHO – Solar and Heliospheric Observatory", "description": "Launched in December 1995, the Solar and Heliospheric Observatory (SOHO) is a joint mission between NASA and ESA (European Space Agency) designed to study the Sun inside out. Though its mission was originally scheduled to last until 1998, SOHO continues to collect observations about the Sun’s interior, the solar atmosphere, and the constant stream of solar particles known as the solar wind, adding to scientists' understanding of our closest star and making many new discoveries, including finding more than 5,000 comets.\n\nLearn more: https://science.nasa.gov/mission/soho/", "hits": 500 }, { "id": 31354, "url": "https://svs.gsfc.nasa.gov/31354/", "result_type": "Animation", "release_date": "2025-06-13T16:19:00-04:00", "title": "PUNCH", "description": "NASA’s PUNCH Releases Its First Images of Huge Eruptions from Sun", "hits": 155 }, { "id": 14509, "url": "https://svs.gsfc.nasa.gov/14509/", "result_type": "Produced Video", "release_date": "2024-02-15T11:00:00-05:00", "title": "How to Safely Watch a Total Solar Eclipse", "description": "On April 8, 2024, a total solar eclipse will cross North America, passing over Mexico, the United States, and Canada. A total solar eclipse happens when the Moon passes between the Sun and Earth, completely blocking the face of the Sun. When watching the partial phases of the solar eclipse it is not safe to look directly at the Sun without safe solar viewing glasses (eclipse glasses) or a safe handheld solar viewer. Eclipse glasses are NOT regular sunglasses; regular sunglasses, no matter how dark, are not safe for viewing the Sun. During the short time when the Moon completely obscures the Sun – known as the period of totality – it is safe to look directly at the star without eye protection. However, it’s crucial that you know when to both remove and put back on your safe solar viewing glasses.To learn more about eclipse safety visit go.nasa.gov/EclipseSafety || ", "hits": 201 }, { "id": 40409, "url": "https://svs.gsfc.nasa.gov/gallery/fermi-stills/", "result_type": "Gallery", "release_date": "2020-01-22T00:00:00-05:00", "title": "Fermi Stills", "description": "A collection of Fermi-related still images, illustrations, graphics and short clips.", "hits": 271 }, { "id": 40360, "url": "https://svs.gsfc.nasa.gov/gallery/sdosolar-events/", "result_type": "Gallery", "release_date": "2018-09-13T09:22:27-04:00", "title": "SDO: Solar Events", "description": "No description available.", "hits": 211 }, { "id": 40355, "url": "https://svs.gsfc.nasa.gov/gallery/sdo/", "result_type": "Gallery", "release_date": "2018-08-31T00:00:00-04:00", "title": "SDO – Solar Dynamics Observatory", "description": "Since its launch on Feb. 11, 2010, the Solar Dynamics Observatory (SDO) has studied the solar atmosphere to help us understand the Sun’s influence on Earth. Every 12 seconds, SDO images the Sun in 10 wavelengths of ultraviolet light, each of which reveals different solar features. These images help us explain where the Sun's energy comes from, how the inside of the Sun works, and how the Sun’s atmosphere stores and releases energy in dramatic eruptions that can influence Earth.\n\nLearn more: https://science.nasa.gov/mission/sdo/", "hits": 800 }, { "id": 4352, "url": "https://svs.gsfc.nasa.gov/4352/", "result_type": "Visualization", "release_date": "2017-08-20T10:00:00-04:00", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (SDO/HMI visible light)", "description": "These movies present the six hour interval around the event, a one minute per animation frame. || MonsterFilament_HMI_stand.HD1080i.00100_print.jpg (1024x576) [40.8 KB] || MonsterFilament_HMI_stand.HD1080i.00100_searchweb.png (320x180) [21.8 KB] || MonsterFilament_HMI_stand.HD1080i.00100_thm.png (80x40) [2.7 KB] || MonsterFilament_HMI_stand.HD1080i.00100_web.png (320x180) [21.8 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || MonsterFilament_HMI.HD1080i_p30.mp4 (1920x1080) [12.1 MB] || MonsterFilament_HMI.HD1080i_p30.webm (1920x1080) [1.2 MB] || MonsterFilament_HMI.HD1080i_p30.mp4.hwshow [197 bytes] || ", "hits": 53 }, { "id": 11667, "url": "https://svs.gsfc.nasa.gov/11667/", "result_type": "Produced Video", "release_date": "2014-09-22T10:00:00-04:00", "title": "The Difference Between CMEs and Flares", "description": "Coronal mass ejections (CMEs) and flares are both solar events, but they are not the same. This video shows the differences between the two by highlighting specific features of each. || ", "hits": 862 }, { "id": 11483, "url": "https://svs.gsfc.nasa.gov/11483/", "result_type": "Produced Video", "release_date": "2014-02-21T09:45:00-05:00", "title": "NASA's IRIS Spots Its Largest Solar Flare", "description": "On Jan. 28, 2014, NASA's Interface Region Imaging Spectrograph, or IRIS, witnessed its strongest solar flare since it launched in the summer of 2013. Solar flares are bursts of x-rays and light that stream out into space, but scientists don't yet know the fine details of what sets them off. IRIS peers into a layer of the sun's lower atmosphere just above the surface, called the chromosphere, with unprecedented resolution. However, IRIS can't look at the entire sun at the same time, so the team must always make decisions about what region might provide useful observations. On Jan. 28, scientists spotted a magnetically active region on the sun and focused IRIS on it to see how the solar material behaved under intense magnetic forces. At 2:40 p.m. EST, a moderate flare, labeled an M-class flare — which is the second strongest class flare after X-class – erupted from the area, sending light and x-rays into space. IRIS studies the layer of the sun’s atmosphere called the chromosphere that is key to regulating the flow of energy and material as they travel from the sun's surface out into space. Along the way, the energy heats up the upper atmosphere, the corona, and sometimes powers solar events such as this flare. IRIS is equipped with an instrument called a spectrograph that can separate out the light it sees into its individual wavelengths, which in turn correlates to material at different temperatures, velocities and densities. The spectrograph on IRIS was pointed right into the heart of this flare when it reached its peak, and so the data obtained can help determine how different temperatures of plasma flow where, giving scientists more insight into how flares work. || ", "hits": 31 }, { "id": 4121, "url": "https://svs.gsfc.nasa.gov/4121/", "result_type": "Visualization", "release_date": "2014-02-11T10:00:00-05:00", "title": "October 2013 X-Flare from Solar Dynamics Observatory", "description": "Another Halloween space weather fest? October-November 2003 of the previous solar cycle saw some of the most energetic solar events since space flight (see Halloween Solar Storms 2003: A Multi-Mission View. Halloween of 2013 has seen a similar round of high solar activity, with energetic flares and coronal mass ejections (CMEs). || ", "hits": 36 }, { "id": 4099, "url": "https://svs.gsfc.nasa.gov/4099/", "result_type": "Visualization", "release_date": "2013-11-04T00:00:00-05:00", "title": "Multiple CMEs of October 2013", "description": "In this research model run, the Sun has launched three coronal mass ejections (CMEs) which may merge into a single front as it expands into the solar system. These events are sometimes called 'cannibal' CMEs.This model run is based on estimated parameters from solar events of October 23-24, 2013 || ", "hits": 49 }, { "id": 40150, "url": "https://svs.gsfc.nasa.gov/gallery/the-cmesof-solar-cycle24/", "result_type": "Gallery", "release_date": "2013-09-25T00:00:00-04:00", "title": "Notable CMEs of Solar Cycle 24", "description": "Simulations & visualizations of some of the big solar events of Solar Cycle 24.\n\nThese visualizations were developed to present a more public-friendly \nview in a way that the major events of space weather, such as coronal \nmass ejections (CMEs) are more obvious even to the untrained observer. \nWe use a fairly basic technique or 'trick' of using the three image \ncolor channels, red, green, and blue, to present different variables \ncomputed in the model run. The visual color-bars are also on the \nanimation page.\n\nIn this case, red represents temperature (kind of obvious choice) so \nredder is hotter plasma. Green represents density of the plasma. Blue \nis a pressure gradient, or change in pressure over distance. More blue \nmeans a stronger shock wave moving through the plasma, which is more a \ncharacteristic of a CME. By combining the three color channels, intense \nvalues of these variables can show up as distinct colors. For example, \na hot, dense shock combines red, green, and blue to form white. But you \ncould also have a lower density hot shock combining red and blue to make \nmagenta (or purple/violet).\n\nThe major visible feature is the 'Parker spiral'. As the solar wind \nflows out from the sun, the sun is rotating. Density enhancements \n(green in the visualization) in the wind get propagated outward to make \nthis spiral shape - not too different from the spiral pattern created by \na spinning lawn sprinkler. Coronal mass ejections get imprinted on this \npattern.", "hits": 61 }, { "id": 4083, "url": "https://svs.gsfc.nasa.gov/4083/", "result_type": "Visualization", "release_date": "2013-06-14T00:00:00-04:00", "title": "CMEpalooza: The Complete Series", "description": "Mid-May 2013 marked a series of active solar events, the likes of which have not been seen since near the peak of solar cycle 23 in October-November of 2003 (see Looking Back at 2003s Spooky Halloween Solar Storms).Five distinct coronal mass ejections, or CMEs, were launched from the sun from Active Regions AR 1748 starting May 13, 2013, through May 20, 2013. Some of the CMEs were associated with preceding M- and X-class flares. The CMEs were not a major threat to Earth technologies as most of them missed Earth, but they did impact various NASA satellites around the solar system. The last of the series of CMEs brushed by Earth. || ", "hits": 72 }, { "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": 120 }, { "id": 3867, "url": "https://svs.gsfc.nasa.gov/3867/", "result_type": "Visualization", "release_date": "2012-09-01T00:00:00-04:00", "title": "A Coronal Mass Ejection strikes Venus!", "description": "Energetic events on the Sun have impacts throughout the Solar System. This visualization, developed for the \"Dynamic Earth\" dome show, opens with a closeup view of the Sun. The solar imagery was collected from the Solar Dynamics Observatory (SDO) using an ultraviolet filter (wavelength 304 Ångstroms or 30.4 nanometers). We can observe jets of ionized gases, called prominences, erupting from the solar surface, and often constrained to loop-shaped trajectories due to the solar magnetic field.We pull out from the Sun to reveal the solar wind, which continuously streams outward from the Sun.We eventually reach the orbit of the planet Venus, the solar wind still streaming around us.But a massive eruption, called a coronal mass ejection, or CME, takes place on the Sun, sending a much higher density of particles (ions and electrons) outward into the solar wind.The wave of particles eventually strikes the planet Venus. But Venus has no significant magnetic field, and the particles make it directly to the atmosphere of the planet. These energetic solar events slowly blow away the atmosphere of the planet.The next part of this sequence is \"The Coronal Mass Ejection strikes the Earth!\".Technical DetailsThis is the dome show component moving from the Sun to Venus being hit by the CME.The domemaster format was created by rendering 7 separate camera tiles. The tiles were then stitched together to form final domemaster layers at 4096x4096 resolution and 16 bits per channel with premultiplied alpha and no gamma correction. There are 3 domemaster layers that should be composited as follows:- Earth and orbits- Sun- star field (no alpha channel)In addition to the final domemaster frames and movies, the individual camera tiles are included as well. Each domemaster layer has a set of camera tiles. There are 7 cameras numbered 00 through 06 that represent the itiles. Camera 00 is in the center of the domemaster, camera 01 is looking below camera 00, cameras 01 through 06 look around the outside of the dome master in counter-clockwise order. These frames are probably only useful if a better re-stitching algorithm is ever required to be run on the tiles. || ", "hits": 56 }, { "id": 11000, "url": "https://svs.gsfc.nasa.gov/11000/", "result_type": "Produced Video", "release_date": "2012-06-11T13:00:00-04:00", "title": "NASA's Fermi Detects the Highest-Energy Light from a Solar Flare", "description": "During a powerful solar blast in March, NASA's Fermi Gamma-ray Space Telescope detected the highest-energy light ever associated with an eruption on the sun. The discovery heralds Fermi's new role as a solar observatory, a powerful new tool for understanding solar outbursts during the sun's maximum period of activity.\"For most of Fermi's four years in orbit, its Large Area Telescope (LAT) saw the sun as a faint, steady gamma-ray source thanks to the impacts of high-speed particles called cosmic rays,\" said Nicola Omodei, an astrophysicist at Stanford University in California. \"Now we're beginning to see what the sun itself can do.\"A solar flare is an explosive blast of light and charged particles. The powerful March 7 flare, which earned a classification of X5.4 based on the peak intensity of its X-rays, is the strongest eruption so far observed by Fermi's LAT. The flare produced such an outpouring of gamma rays — a form of light with even greater energy than X-rays — that the sun briefly became the brightest object in the gamma-ray sky.At the flare's peak, the LAT detected gamma rays with two billion times the energy of visible light, or about 4 billion electron volts (GeV), easily setting a record for the highest-energy light ever detected during or just after a solar flare. The flux of high-energy gamma rays, defined as those with energies beyond 100 million electron volts (MeV), was 1,000 times greater than the sun's steady output. The March 7 flare also is notable for the persistence of its gamma-ray emission. Fermi's LAT detected high-energy gamma rays for about 20 hours, two and a half times longer than any event on record. Additionally, the event marks the first time a greater-than-100-MeV gamma-ray source has been localized to the sun's disk, thanks to the LAT's keen angular resolution. Flares and other eruptive solar events produce gamma rays by accelerating charged particles, which then collide with matter in the sun's atmosphere and visible surface. For instance, interactions among protons result in short-lived subatomic particles called pions, which produce high-energy gamma rays when they decay. Nuclei excited by collisions with lower-energy ions give off characteristic gamma rays as they settle down. Accelerated electrons emit gamma rays as they collide with protons and atomic nuclei.Solar eruptions are now on the rise as the sun progresses toward the peak of its roughly 11-year-long activity cycle, now expected in mid-2013. || ", "hits": 86 }, { "id": 10941, "url": "https://svs.gsfc.nasa.gov/10941/", "result_type": "Produced Video", "release_date": "2012-04-24T10:00:00-04:00", "title": "Space Weather FAQ Interviews", "description": "NASA scientists answer some frequently asked questions about the sun, space weather, and the effects on Earth. Each video is one or more scientists responding to the question above it. The videos are available as ProRes files for broadcast use and have had minor audio equalizing and color correction applied.The scientists interviewed are:Dr. Holly Gilbert, NASA HeliophysicistDr. Alex Young, NASA HeliophysicistDr. Phil Chamberlin, NASA Research Heliophysicist and SDO Deputy Project ScientistThere are also two short videos created with this interview content. They are available here.Additional responses to these questions are available upon specific request.For space weather-related footage, animations, and features, visit the Space Weather gallery. || ", "hits": 27 }, { "id": 40117, "url": "https://svs.gsfc.nasa.gov/gallery/sun-news/", "result_type": "Gallery", "release_date": "2012-04-04T00:00:00-04:00", "title": "Heliophysics Breaking News", "description": "This gallery contains an archive of breaking news solar events such as flares, CMEs, solar storms, and comet passes. The most recent material is at the top left, and it progresses back in time left-to-right and top-down. Each page contains video and/or stills of a distinct event or series of linked events.The videos are available at multiple resolutions and compressions, including Apple ProRes 422. Where applicable, there are links to 4k x 4k tif frames.For sun-related background, animations, visualizations and informational content, go here.For pre-recorded, frequently-asked-question interviews with NASA scientists, go here.", "hits": 194 }, { "id": 40115, "url": "https://svs.gsfc.nasa.gov/gallery/space-weather/", "result_type": "Gallery", "release_date": "2011-12-01T00:00:00-05:00", "title": "Space Weather", "description": "The term \"space weather\" was coined not long ago to describe the dynamic conditions in the Earth's outer space environment, in the same way that \"weather\" and \"climate\" refer to conditions in Earth's lower atmosphere. Space weather includes any and all conditions and events on the sun, in the solar wind, in near-Earth space and in our upper atmosphere that can affect space-borne and ground-based technological systems and through these, human life and endeavor. Heliophysics is the science of space weather.\r\n\r\nThis gallery organizes satellite footage, animations, visualizations, and edited videos produced at the Goddard Space Flight Center. Visualizations are different from pure animations because they are data-driven. They present a way of \"seeing\" the data. In the case of orbit visualizations, they are based on actual orbit information. Most of the animations and visualizations are available as frames and all the recent ones are HD quality. All videos are available in several formats and qualities including Apple ProRes for broadcast quality. Unless specifically marked otherwise, all these materials are public domain and free to use. For more infomation about NASA's media use guidelines see this page.\r\n\r\nThe content is organized in two ways. Under \"Facets of Space Weather\" you will find our visuals grouped by the subject they address. Under \"NASA Spacecraft\" you will find our visuals grouped by the satellite they were collected by, or that they refer to. This group also contains animations of the spacecraft themselves.\r\nFor breaking news solar events, go to this gallery.For frequently-asked-question interviews with NASA scientists, go here.", "hits": 115 }, { "id": 10821, "url": "https://svs.gsfc.nasa.gov/10821/", "result_type": "Produced Video", "release_date": "2011-09-13T00:00:00-04:00", "title": "Sun's Weather Encompasses Earth", "description": "The sun regularly spews forth bursts of particles and magnetic fields known as a coronal mass ejection, or, CME. A CME starts small in solar terms—just a few hundred times the size of the Earth—but it grows and changes as it travels toward the edges of the solar system. Scientists have been observing these events with satellites for decades, but tracking the details of an ejection's growth from original seed to complex structure near Earth has been more challenging. In fact, scientists recently used three NASA spacecraft—STEREO-A, WIND and ACE—to create the first visual record of a CME's path from the sun to the Earth. The orbiting instruments captured the CME's birth on Dec. 12, 2008 at the sun's surface, its exponential growth and its ultimate engulfing of the Earth about three days later. These ejections are common but large solar events can alter our magnetic atmosphere to such a degree that communications signals from GPS or telecom satellites are temporarily degraded beyond recognition. This visualization allowed scientists to watch how features early in the CME ultimately create the form seen closer to Earth, with a bright leading edge and trailing evacuated cavity. || ", "hits": 38 }, { "id": 3838, "url": "https://svs.gsfc.nasa.gov/3838/", "result_type": "Visualization", "release_date": "2011-07-01T10:00:00-04:00", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (304 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3840 (211 Ångstroms) and 3841 (1700 Ångstroms). || ", "hits": 74 }, { "id": 3839, "url": "https://svs.gsfc.nasa.gov/3839/", "result_type": "Visualization", "release_date": "2011-07-01T10:00:00-04:00", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (171 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3838 (304 Ångstroms), 3840 (211 Ångstroms) and 3841 (1700 Ångstroms). || ", "hits": 53 }, { "id": 3840, "url": "https://svs.gsfc.nasa.gov/3840/", "result_type": "Visualization", "release_date": "2011-07-01T10:00:00-04:00", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (211 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). Much of the ejected material is much cooler (less than about 80,000K) and therefore appears dark against the brighter solar disk.Material which does not reach solar escape velocity can be seen falling back and striking the solar surface, sometimes triggering smaller events.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3838 (304 Ångstroms) and 3841 (1700 Ångstroms). || ", "hits": 45 }, { "id": 3841, "url": "https://svs.gsfc.nasa.gov/3841/", "result_type": "Visualization", "release_date": "2011-07-01T10:00:00-04:00", "title": "Incredible Solar Flare, Prominence Eruption and CME Event (1700 angstroms)", "description": "On June 7, 2011, an M-2 flare occurred on the Sun which released a very large coronal mass ejection (CME). At this wavelength, very little of the ejected material is visible. However, it is possible to see locations where some of the material is falling back and striking the solar surface.This image sequence is captured at one minute intervals and designed to play synchronously with animations 3839 (171 Ångstroms), 3840 (211 Ångstroms) and 3838 (304 Ångstroms). || ", "hits": 47 }, { "id": 10623, "url": "https://svs.gsfc.nasa.gov/10623/", "result_type": "Produced Video", "release_date": "2010-07-29T00:00:00-04:00", "title": "Rebounding Plasma Flows in the Inner Magnetosphere", "description": "Substorms send jets of plasma careening Earthward at speeds near 600,000 miles/hour. Researchers comparing multipoint THEMIS spacecraft observations with the predictions of numerical simulations have determined the width of one such jet and determined what happened to it when it encountered the strong magnetic fields within the inner magnetosphere. Plasma jets with the width of the Earth slam into the inner magnetosphere, generating vortices with opposite senses of rotation that appear and disappear on either side of the plasma jet. These vortices become sources of field-aligned electrical currents that flow down to the Earth's ionosphere, where they generate auroral brightenings and intense magnetic field disturbances. After striking the inner magnetospheric magnetic field, the plasma jet itself bounces back and forth, losing energy each time it encounters the magnetic field, and continuing to oscillate until the flow energy is dissipated in the form of plasma heating. || ", "hits": 61 }, { "id": 3683, "url": "https://svs.gsfc.nasa.gov/3683/", "result_type": "Visualization", "release_date": "2010-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: GOES/SXI X-ray view", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The GOES-12/Solar X-Ray Imager was experiencing significant problems during this time period and was offline during part of the opening and closing portions of this movie, which is why there is a significant number of black frames. Actual data collection began on October 28, 2003 and terminated on November 5, 2003.This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstromsHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromsHalloween 2003 Solar Storms: SOHO/MDI ContinuumHalloween 2003 Solar Storms: SOHO/MDI MagnetogramsHalloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO || ", "hits": 29 }, { "id": 3595, "url": "https://svs.gsfc.nasa.gov/3595/", "result_type": "Visualization", "release_date": "2009-07-27T00:00:00-04:00", "title": "Sentinels of the Heliosphere", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point, a point between the Earth and the Sun where the gravitational pull is approximately equal. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageThis enhanced, narrated visualization was shown at the SIGGRAPH 2009 Computer Animation Festival in New Orleans, LA in August 2009; an eariler version created for AGU was called NASA's Heliophysics Observatories Study the Sun and Geospace. || ", "hits": 104 }, { "id": 10421, "url": "https://svs.gsfc.nasa.gov/10421/", "result_type": "Produced Video", "release_date": "2009-04-07T00:00:00-04:00", "title": "SOHO/TRACE Intro", "description": "On April 3, 2009, countries from around the world participated in the '100 Hours of Astronomy' webcast to celebrate the International Year of Astronomy. This movie was used to introduce the SOHO/TRACE segment. Alex Young and Dawn Meyers, NASA scientists, describe how both SOHO and TRACE view the sun in their own unique way. || ", "hits": 32 }, { "id": 3570, "url": "https://svs.gsfc.nasa.gov/3570/", "result_type": "Visualization", "release_date": "2008-12-15T00:00:00-05:00", "title": "NASA's Heliophysics Observatories Study the Sun and Geospace", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point between the Sun and the Earth. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageA refined and narrated version of this visualization, Sentinels of the Heliosphere, is now available. || ", "hits": 97 }, { "id": 3500, "url": "https://svs.gsfc.nasa.gov/3500/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 Angstroms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 195 angstroms corresponds (19.5 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 A Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 30 }, { "id": 3501, "url": "https://svs.gsfc.nasa.gov/3501/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 Angstroms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Extreme ultraviolet Imaging Telescope (EIT) collects solar images in an extremely short wavelength of ultraviolet light, not visible from the surface of the Earth. The narrow wavelength band at 304 Ångstroms corresponds (30.4 nanometers) corresponds to a spectral line of multiply-ionized iron atoms. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 ÅHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 54 }, { "id": 3502, "url": "https://svs.gsfc.nasa.gov/3502/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/MDI Continuum", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The Michelson Doppler Interferometer (MDI) records images at several very narrow wavelength bands in the visible light. These images are often used as proxies for white-light solar images. This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 13 }, { "id": 3504, "url": "https://svs.gsfc.nasa.gov/3504/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO", "description": "Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera.This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstromHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms For more information, visit the SOHO project page.. || ", "hits": 47 }, { "id": 3431, "url": "https://svs.gsfc.nasa.gov/3431/", "result_type": "Visualization", "release_date": "2007-05-29T00:00:00-04:00", "title": "Coronal Mass Ejections (CME): Radio Quiet Variety", "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image. Moving material therefore appears white on the leading edge and dark behind it. The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis). A vertical white bar marks the time of the LASCO image.This CME shows no radio-loud emission between 0.2-1.0 MHz. || ", "hits": 24 }, { "id": 3432, "url": "https://svs.gsfc.nasa.gov/3432/", "result_type": "Visualization", "release_date": "2007-05-29T00:00:00-04:00", "title": "Coronal Mass Ejections (CME): Radio Loud Variety", "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image. Moving material therefore appears white on the leading edge and dark behind it. The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis). A vertical white bar marks the time of the LASCO image.The radio-loud emission of the CME is the yellow-orange band between 0.2-1.0 MHz. || ", "hits": 33 }, { "id": 3159, "url": "https://svs.gsfc.nasa.gov/3159/", "result_type": "Visualization", "release_date": "2005-05-24T12:00:00-04:00", "title": "SOHO/LASCO View of January 2005 Solar Events", "description": "The January 20 flare began just before 2 a.m. ET. A storm of energetic protons impacted Earth just 15 minutes later. These views of the flare are from the Solar and Heliospheric Observatory (SOHO). The proton storm near Earth causes `snow' in the images, obscuring the Sun as radiation swamps the cameras. The structure at the 1:30 position in the SOHO/LASCO/C3 data is the occulting disk pylon. || ", "hits": 22 }, { "id": 2959, "url": "https://svs.gsfc.nasa.gov/2959/", "result_type": "Visualization", "release_date": "2004-07-08T12:00:00-04:00", "title": "Halloween Solar Storms from SOHO/EIT, 195 Angstroms", "description": "This view from SOHO/EIT in the 195 angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 and 2961. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ", "hits": 19 } ] }