{ "count": 15, "next": null, "previous": null, "results": [ { "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": 177 }, { "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": 59 }, { "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": 68 }, { "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": 57 }, { "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": 51 }, { "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": 43 }, { "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": 68 }, { "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": 32 }, { "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": 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": 37 }, { "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": 53 }, { "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": 27 }, { "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": 48 }, { "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": 23 }, { "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": 45 } ] }