{ "count": 12, "next": null, "previous": null, "results": [ { "id": 12200, "url": "https://svs.gsfc.nasa.gov/12200/", "result_type": "Produced Video", "release_date": "2017-07-25T15:00:00-04:00", "title": "Solar Eclipse Safety Images", "description": "People watch a partial eclipse in Belfast, Northern Ireland, on Mar. 20, 2015. Credit: Robin Cordiner || RobinCordiner.jpg (926x618) [118.5 KB] || RobinCordinerlg_print.jpg (1024x683) [681.3 KB] || RobinCordinerlg.jpg (7065x4715) [22.0 MB] || RobinCordinerlg_searchweb.png (320x180) [98.8 KB] || RobinCordinerlg_web.png (320x213) [114.5 KB] || RobinCordinerlg_thm.png (80x40) [6.7 KB] || ", "hits": 74 }, { "id": 12183, "url": "https://svs.gsfc.nasa.gov/12183/", "result_type": "Produced Video", "release_date": "2016-03-24T13:10:18-04:00", "title": "Solar Outburst", "description": "A NASA spacecraft sees a spectacular explosion on the sun. || c-1024.jpg (1024x576) [142.6 KB] || c-1280.jpg (1280x720) [184.3 KB] || c-1024_print.jpg (1024x576) [155.2 KB] || c-1024_searchweb.png (320x180) [88.7 KB] || c-1024_web.png (320x180) [88.7 KB] || c-1024_thm.png (80x40) [20.6 KB] || ", "hits": 36 }, { "id": 11805, "url": "https://svs.gsfc.nasa.gov/11805/", "result_type": "Produced Video", "release_date": "2015-03-11T14:00:00-04:00", "title": "Sun Emits an X2.2 Flare on March 11, 2015", "description": "An X2.2 class solar flare flashes in the middle of the sun on Mar. 11, 2015. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 171 and 131 angstrom wavelengths.Credit: NASA/GSFC/SDO || March_11_2015_X2pt2_Flare_171-131-crop_2.png (1920x1200) [12.7 MB] || March_11_2015_X2pt2_Flare_171-131-crop_2.jpg (1920x1200) [682.3 KB] || March_11_2015_X2pt2_Flare_171-131-crop_2_print.jpg (1024x640) [168.4 KB] || March_11_2015_X2pt2_Flare_171-131-crop_2_web.jpg (320x200) [24.0 KB] || March_11_2015_X2pt2_Flare_171-131-crop_2_searchweb.png (320x180) [118.6 KB] || March_11_2015_X2pt2_Flare_171-131-crop_2_thm.png (80x40) [10.5 KB] || ", "hits": 54 }, { "id": 11705, "url": "https://svs.gsfc.nasa.gov/11705/", "result_type": "Produced Video", "release_date": "2014-10-06T14:00:00-04:00", "title": "NASA's SDO Watches Giant Filament on the Sun", "description": "A snaking, extended filament of solar material currently lies on the front of the sun— some 1 million miles across from end to end. Filaments are clouds of solar material suspended above the sun by powerful magnetic forces. Though notoriously unstable, filaments can last for days or even weeks.NASA's Solar Dynamics Observatory, or SDO, which watches the sun 24 hours a day, has observed this gigantic filament for several days as it rotated around with the sun. If straightened out, the filament would reach almost across the whole sun, about 1 million miles or 100 times the size of Earth.SDO captured images of the filament in numerous wavelengths, each of which helps highlight material of different temperatures on the sun. By looking at any solar feature in different wavelengths and temperatures, scientists can learn more about what causes such structures, as well as what catalyzes their occasional giant eruptions out into space.Look at the images to see how the filament appears in different wavelengths. The brownish combination image was produced by blending two wavelengths of extreme UV light with a wavelength of 193 and 335 angstroms. The red image shows the 304 angstrom wavelength of extreme UV light. || ", "hits": 62 }, { "id": 30481, "url": "https://svs.gsfc.nasa.gov/30481/", "result_type": "Infographic", "release_date": "2013-12-02T10:00:00-05:00", "title": "Heliophysics and Space Weather", "description": "The sun and its atmosphere consist of several zones, or layers, from the inner core to the outer corona. Beyond the corona is the solar wind, which is an outward expansion of coronal plasma that extends well beyond the orbit of Pluto. This entire region of space influenced by the sun is called the heliosphere. Controlled by the Earth’s magnetic field, the magnetosphere acts as a shield protecting the planet from solar wind. The shape of the Earth's magnetosphere is the direct result of being impacted by solar wind, compressed on its sunward side and elongated on the night-side, the magnetotail. The shock wave where the solar wind encounters Earth's magnetosphere is called the bow shock, which slows and diverts the solar wind. Solar activity lead to solar eruptions, which includes such phenomena as sunspots, flares, prominences, and coronal mass ejections that influence space weather, or near-Earth environmental conditions. Modern society depends heavily on a variety of technologies that are susceptible to space weather. CMEs for example can cause geomagnetic storms that can disrupt satellite communications and navigational equipment, and even cause blackouts. || ", "hits": 184 }, { "id": 11257, "url": "https://svs.gsfc.nasa.gov/11257/", "result_type": "Produced Video", "release_date": "2013-04-26T16:00:00-04:00", "title": "CMEs Galore", "description": "On April 20, 2013, at 2:54 a.m. EDT, the sun erupted with a coronal mass ejection (CME), a solar phenomenon that can send billions of tons of solar particles into space that can affect electronic systems in satellites. Experimental NASA research models show that the CME left the sun at 500 miles per second and is not Earth-directed. However, it may pass by NASA's Messenger and STEREO-A satellites, and their mission operators have been notified. There is, however, no particle radiation associated with this event, which is what would normally concern operators of interplanetary spacecraft since the particles can trip computer electronics on board. When warranted, NASA operators can put spacecraft into safe mode to protect the instruments from the solar material. The same region of the sun erupted with another coronal mass ejection (CME) at 3:54 a.m. on April 21, 2013. Experimental NASA research models show the CME left the sun at speeds of 550 miles per second. The models show that the CME will also pass by NASA's Messenger and the flank of the CME may graze STEREO-A.Another coronal mass ejection (CME) has erupted from the sun, headed toward Mercury and NASA's Messenger spacecraft. The CME began at 12:39 p.m. EDT on April 21, 2013. Experimental NASA research models show that the CME left the sun at 625 miles per second and that it will catch up to the CME from earlier on April 21 before the combined CMEs pass Messenger. There is also chance that the combined CMEs will give a glancing blow to STEREO-A. || ", "hits": 145 }, { "id": 10972, "url": "https://svs.gsfc.nasa.gov/10972/", "result_type": "Produced Video", "release_date": "2012-05-10T00:00:00-04:00", "title": "Greatest Hits", "description": "Ever since NASA's Solar Dynamics Observatory (SDO) began collecting images in April 2010, it has delivered incredible views of the sun ranging from stunning to downright explosive. In the past two years, the sun generated more than 1,000 outbursts, including solar flares, coronal mass ejections and energetic particles that travel to the edge of the solar system. By recording these events in multiple wavelengths, scientists can unravel the process by which the roiling magnetic fields inside and around the sun cause it to erupt. For example, the above image showing light at 171 Angstroms and colorized in gold reveals the looping arcs of particles that coalesce around magnetic field lines in the sun's atmosphere during intense periods of solar activity. Other wavelengths make different features more readily visible to the human eye. Watch the video below highlighting some of the most amazing moments witnessed by SDO in its second year of operation. || ", "hits": 30 }, { "id": 10966, "url": "https://svs.gsfc.nasa.gov/10966/", "result_type": "Produced Video", "release_date": "2012-04-20T08:00:00-04:00", "title": "SDO: Year 2", "description": "April 21, 2012 marks the two-year anniversary of the Solar Dynamics Observatory (SDO) First Light press conference, where NASA revealed the first images taken by the spacecraft. This video highlights just some of the amazing events witnessed in SDO's second year. || ", "hits": 33 }, { "id": 10784, "url": "https://svs.gsfc.nasa.gov/10784/", "result_type": "Produced Video", "release_date": "2011-07-27T08:00:00-04:00", "title": "Revealing the Old Man in the Sun", "description": "When one moves through 11 SDO images taken at the same time, and shown in order from the lowest temperature material being imaged to the highest, a funny thing thing happens: the features of a face in the sun begin to appear. The movie underscores the fact that images taken at different wavelengths do reveal different features. The images also start at the sun's surface and gradually move out to the sun's upper corona. Enjoy the show! || ", "hits": 32 }, { "id": 3548, "url": "https://svs.gsfc.nasa.gov/3548/", "result_type": "Visualization", "release_date": "2008-09-10T00:00:00-04:00", "title": "Comparison: Solar Minimum from SOHO/EIT", "description": "This is a short movie of the Sun at the minimum of solar activity. This images are collected in ultraviolet light (a wavelength of 195 Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, few to now sunspots would be visible.At solar minimum, we see few bright active regions. The mottled look is from small 'hot spots' which last less than 48 hours. There are dark regions at the top and bottom of the Sun (corresponding to the north and south solar poles) created by solar magnetic field lines that connect to the interstellar magnetic field. A similar dark region, below the solar equator, is called a coronal hole, where open magnetic field lines enable particles to stream away at high speeds. || ", "hits": 33 }, { "id": 3549, "url": "https://svs.gsfc.nasa.gov/3549/", "result_type": "Visualization", "release_date": "2008-09-10T00:00:00-04:00", "title": "Comparison: Solar Maximum from SOHO/EIT", "description": "A short movie of the Sun at maximum solar activity as seen in ultraviolet light. These images are collected in ultraviolet light (a wavelength of 195Å or 19.5 nanometers) which is only visible to space-based instruments. In visible light, the bright white regions in these images would probably correspond to sunspots.At solar maximum, we see many bright active regions which tend to form in bands in the northern and southern hemispheres. Many of the active regions may eventually launch solar flares or coronal mass ejections (CME). || ", "hits": 28 }, { "id": 3386, "url": "https://svs.gsfc.nasa.gov/3386/", "result_type": "Visualization", "release_date": "2006-11-08T00:00:00-05:00", "title": "Mercury Transit from SOHO/MDI", "description": "This is a view of the planet Mercury (the tiny moving black dot) as seen by the SOHO MDI.The narrow field-of-view for this camera mode necessitates the addition of black bars at the top and bottom of the frame to match HD720 resolution.This movie was generated from telemetry which has undergone a minimum of processing (to deliver quickly for the media) so data dropouts and other quick-processing artifacts may be visible. Special thanks to Steele Hill of the SOHO project for this effort. || ", "hits": 25 } ] }