{ "count": 85, "next": null, "previous": null, "results": [ { "id": 15011, "url": "https://svs.gsfc.nasa.gov/15011/", "result_type": "Produced Video", "release_date": "2026-05-01T11:00:00-04:00", "title": "NASA Experiment to Track Space ‘Doughnut’ Encircling Earth", "description": "NASA is launching a new experiment to track charged particles in a \"space doughnut\" that encircles our planet. Installed on the exterior of the International Space Station, the new experiment will study the ring current — a doughnut-shaped swarm of particles that can surge when a solar blast hits Earth, disrupting our satellites in space and power systems on the ground.", "hits": 869 }, { "id": 15013, "url": "https://svs.gsfc.nasa.gov/15013/", "result_type": "Produced Video", "release_date": "2026-05-01T09:00:00-04:00", "title": "STORIE Prepares for Launch at Kennedy Space Center", "description": "NASA’s STORIE (Storm Time O+ Ring current Imaging Evolution) instrument is shown here installed on the Space Test Program – Houston 11 (STP-H11) payload, a partnership between the U.S. Space Force and NASA, at the Space Station Processing Facility at NASA's Kennedy Space Center in Florida. It is covered in blanketing material to protect STORIE from the space environment. After launch, the STP-H11 payload and STORIE will be installed on the outside of the International Space Station’s Columbus module.Learn more: https://science.nasa.gov/science-research/heliophysics/nasas-storie-mission-to-tell-tale-of-earths-ring-current/ || ", "hits": 2291 }, { "id": 31389, "url": "https://svs.gsfc.nasa.gov/31389/", "result_type": "Hyperwall Visual", "release_date": "2026-04-08T12:00:00-04:00", "title": "How Atoms Are Defying Gravity in NASA's Cold Atom Lab", "description": "NASA’s Cold Atom Lab studies the quantum nature of atoms, the building blocks of our universe, in a place that is out of this world – the International Space Station. This animated explainer explores what quantum science is and why NASA wants to do it in space.", "hits": 469 }, { "id": 14991, "url": "https://svs.gsfc.nasa.gov/14991/", "result_type": "Produced Video", "release_date": "2026-03-20T12:00:00-04:00", "title": "Argonne Assembles, Tests Early ComPair-2 Hardware", "description": "Tim Cundiff, an engineering specialist at Argonne National Laboratory in Lemont, Illinois, monitors the automated wire bond of a ComPair-2 detector layer in April 2025. Image courtesy of Argonne National LaboratoryAlt text: A man in a lab uses a microscope.Image description: A man in a white clean suit, gloves, safety glasses, and a hairnet sits in front of a piece of machinery in a laboratory and peers into a microscope. Behind him is a long bench covered in scientific equipment and computers. In front of him, inside the machinery, are what look like two black treads that loop in and out of frame. || 34340D_0388_PSE_NASA_Goddard_Gamma-Ray_Tracker_Assembly_Process_WEB_16x9.jpg (2000x1125) [1.1 MB] || 34340D_0388_PSE_NASA_Goddard_Gamma-Ray_Tracker_Assembly_Process_WEB_16x9_searchweb.png (320x180) [124.6 KB] || 34340D_0388_PSE_NASA_Goddard_Gamma-Ray_Tracker_Assembly_Process_WEB_16x9_thm.png (80x40) [27.3 KB] || ", "hits": 91 }, { "id": 14980, "url": "https://svs.gsfc.nasa.gov/14980/", "result_type": "Produced Video", "release_date": "2026-02-26T12:00:00-05:00", "title": "Prototype ComPair-2 Gamma-Ray Detectors Complete Thermal Vacuum Testing", "description": "Prototype gamma-ray detectors for the ComPair-2 mission rests in a thermal vacuum chamber after testing in June 2025 at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. The ComPair-2 team tested the detectors’ performance at hot and cold temperatures over the course of a week and the overall survivability of the layer itself. Credit: NASA/Sophia RobertsAlt text: A piece of equipment sits inside a chamber in a lab. Image description: A cylindrical metal chamber at the center of the image has its door swung all the way open. Inside are silver-wrapped ComPair-2 detectors attached to many copper-colored wires. The chamber is in a lab with white walls and has tubes, wires, and other pieces of equipment attached. || ComPair2_TVAC-1-small.jpg (4096x2732) [3.2 MB] || ComPair2_TVAC-1.jpg (8192x5464) [30.6 MB] || ", "hits": 76 }, { "id": 14955, "url": "https://svs.gsfc.nasa.gov/14955/", "result_type": "Produced Video", "release_date": "2026-01-27T09:00:00-05:00", "title": "NASA Tests LISA Development Units", "description": "A prototype charge management device for the future LISA (Laser Interferometer Space Antenna) mission sits on a lab bench at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. The device will reduce the buildup of electric charge on the gold-platinum test masses that float freely inside each of the three LISA spacecraft. The University of Florida in Gainesville and Fibertek Inc. in McNair, Virginia, are developing the device. Credit: NASA/Dennis HenryAlt text: An instrument rests on a lab bench.Image description: A silver box with red and black connector caps on one side rests on a white lab bench with a blue mat on top. Three black cables connect to the box and another yellow cable curls around it. || GSFC_20250602_LISA_006584.jpg (8098x5399) [11.3 MB] || ", "hits": 251 }, { "id": 14874, "url": "https://svs.gsfc.nasa.gov/14874/", "result_type": "Produced Video", "release_date": "2025-07-28T10:00:00-04:00", "title": "STORIE Thermal Vacuum Test at NASA Goddard Space Flight Center", "description": "NASA’s STORIE mission, or Storm Time O+ Ring current Imaging Evolution, has completed its design, build, and testing campaign at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, ahead of its six-month mission onboard the International Space Station (ISS). From its unique vantage point on the ISS, STORIE will use its onboard neutral atom imager to provide an “inside out” view of Earth’s ring current – a region of the magnetosphere where energetic particles are trapped in near-Earth space. In addition to answering fundamental questions about the ring current’s intensity and composition, STORIE will also provide a more detailed understanding of how geomagnetic storms affect Earth.From NASA’s Goddard Space Flight Center, STORIE will be shipped to NASA’s Johnson Space Center in Houston, Texas, where it will be integrated onto a pallet to be installed outside the ISS’s Columbus Module. STORIE will head to the ISS aboard a SpaceX commercial resupply flight no earlier than spring 2026. || ", "hits": 180 }, { "id": 5567, "url": "https://svs.gsfc.nasa.gov/5567/", "result_type": "Visualization", "release_date": "2025-07-21T18:59:59-04:00", "title": "New Missions to L1", "description": "Three missions, Carruthers, IMAP and SWFO-L1 will be launched to the Sun-Earth Lagrange Point, L1.", "hits": 179 }, { "id": 14869, "url": "https://svs.gsfc.nasa.gov/14869/", "result_type": "Produced Video", "release_date": "2025-07-18T11:00:00-04:00", "title": "STORIE Fit Test at NASA Goddard Space Flight Center", "description": "NASA’s STORIE mission, or Storm Time O+ Ring current Imaging Evolution, has completed its design, build, and testing campaign at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, ahead of its mission onboard the International Space Station (ISS). From its unique vantage point on the ISS, STORIE will use neutral atom imaging to provide an “inside out” view of Earth’s ring current – a region of the magnetosphere where energetic particles are trapped in near-Earth space. In addition to answering fundamental questions about the ring current’s intensity and composition, STORIE will also provide a more detailed understanding of how geomagnetic storms affect Earth.From NASA’s Goddard Space Flight Center, STORIE will be shipped to NASA’s Johnson Space Center in Houston, Texas, where it will be integrated onto a pallet to be installed outside the ISS’s Columbus Module. STORIE will head to the ISS aboard a SpaceX commercial resupply flight no earlier than spring 2026. || ", "hits": 89 }, { "id": 20403, "url": "https://svs.gsfc.nasa.gov/20403/", "result_type": "Animation", "release_date": "2025-05-14T09:00:00-04:00", "title": "Titan science results from James Webb Space Telescope: animation resource page", "description": "Push into JWST to Saturn and Titan. || JWST_Titan_Intro_Final_V001.00957_print.jpg (1024x576) [145.8 KB] || JWST_Titan_Intro_Final_V001.00957_searchweb.png (320x180) [78.0 KB] || JWST_Titan_Intro_Final_V001.00957_thm.png [5.5 KB] || JWST_Titan_Intro_Final_1080.mp4 (1920x1080) [72.8 MB] || JWST_Titan_Intro_Final_V001.mp4 (3840x2160) [38.4 MB] || JWST_Titan_Intro_Final_V001.mov (3840x2160) [6.8 GB] || ", "hits": 193 }, { "id": 14811, "url": "https://svs.gsfc.nasa.gov/14811/", "result_type": "Produced Video", "release_date": "2025-04-02T00:00:00-04:00", "title": "IMAP: Mapping The Heliosphere & Sun", "description": "The Interstellar Mapping and Acceleration Probe, or IMAP, will explore and map the very boundaries of our heliosphere — a huge bubble created by the Sun's wind that encapsulates our entire solar system — and study how the heliosphere interacts with the local galactic neighborhood beyond.The mission’s investigation of the boundaries of the heliosphere will be primarily done with energetic neutral atoms, or ENAs. An ENA is a type of uncharged particle formed when an energetic positively charged ion runs into a slow-moving neutral atom. The ion picks up an extra negatively charged electron in the collision, making it neutral — hence the name energetic neutral atom. This process frequently happens wherever there is plasma in space, such as throughout the heliosphere, including its boundary.The IMAP-Lo, IMAP-HI, and IMAP-Ultra instruments on IMAP are imaging the energies and composition of ENAs.Learn more about IMAP: https://science.nasa.gov/mission/imap/ || ", "hits": 137 }, { "id": 14794, "url": "https://svs.gsfc.nasa.gov/14794/", "result_type": "Produced Video", "release_date": "2025-03-11T00:00:00-04:00", "title": "Developing NASA’s ComPair-2 Detectors", "description": "ComPair-2 will host a gamma-ray tracker with 10 layers, each with 380 silicon detectors, like the engineering test unit shown here. This trial version allows the mission team to test the electronics, measure how well the detectors work together, and develop assembly procedures for each layer. Credit: NASA/Sophia RobertsAlt text: Scientific hardware on a table Image description: A square piece of scientific hardware rests on a table on top of a silver cover. The hardware has a white board on the bottom with a silver peg at each corner. Inside the pegs is a black square with orange and green electronic components. The green runs along the bottom of the square and takes up the left corner of the black square. The orange electronic components run in 20 stripes along the black square. The orange is interspersed with black. || ComPair2-3_print.jpg (1024x683) [631.9 KB] || ComPair2-3.jpg (8192x5464) [29.1 MB] || ComPair2-3_searchweb.png (320x180) [124.5 KB] || ComPair2-3_web.png (320x213) [137.6 KB] || ComPair2-3_thm.png [28.0 KB] || ", "hits": 40 }, { "id": 14628, "url": "https://svs.gsfc.nasa.gov/14628/", "result_type": "Produced Video", "release_date": "2024-08-28T11:30:00-04:00", "title": "Discovering Earth’s Third Global Energy Field", "description": "High above the Earth’s North and South Poles, a steady stream of particles escapes from our atmosphere into space. Scientists call this mysterious outflow the “polar wind,” and for almost 60 years, spacecraft have been flying through it as scientists have theorized about its cause. The leading theory was that a planet-wide electric field was drawing those particles up into space. But this so-called ambipolar electric field, if it exists, is so weak that all attempts to measure it have failed – until now.In 2022, scientists traveled to Svalbard, a small archipelago in Norway, to launch a rocket in an attempt to measure Earth’s ambipolar electric field for the first time. This was NASA’s Endurance rocketship mission, and this is its story.To learn more, visit: https://science.nasa.gov/science-research/heliophysics/nasa-discovers-long-sought-global-electric-field-on-earth/ || ", "hits": 352 }, { "id": 5153, "url": "https://svs.gsfc.nasa.gov/5153/", "result_type": "Visualization", "release_date": "2023-09-26T17:00:00-04:00", "title": "Carbon Monoxide (CO)", "description": "Near surface concentration of carbon monoxide (CO) estimated by NASA’s GEOS-CF model.", "hits": 107 }, { "id": 14373, "url": "https://svs.gsfc.nasa.gov/14373/", "result_type": "Infographic", "release_date": "2023-08-08T10:00:00-04:00", "title": "ComPair Infographic", "description": "Explore this infographic to learn more about ComPair and scientific ballooning.Credit: NASA’s Goddard Space Flight CenterMachine-readable PDF copy || ComPair_Infographic_Final.jpg (5100x6600) [3.3 MB] || ComPair_Infographic_Final.png (5100x6600) [11.7 MB] || ComPair_Infographic_Final-half.jpg (2550x3300) [1.3 MB] || ComPair_Infographic_Final-half.png (2550x3300) [3.8 MB] || ", "hits": 48 }, { "id": 14354, "url": "https://svs.gsfc.nasa.gov/14354/", "result_type": "B-Roll", "release_date": "2023-05-25T00:00:00-04:00", "title": "ComPair Gamma-Ray Balloon Mission", "description": "Carolyn Kierans, principal investigator for the ComPair balloon mission at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, works on the instrument in this video. First, she assembles a layer of the tracker, which is housed in an aluminum casing. Next, she shows one of the tracker’s silicon detectors. Then she takes the lid off the tracker.Credit: NASA/Sophia Roberts || Unassembled_Parts_of_ComPair.01740_print.jpg (1024x540) [148.3 KB] || Unassembled_Parts_of_ComPair.01740_searchweb.png (320x180) [94.0 KB] || Unassembled_Parts_of_ComPair.01740_thm.png (80x40) [7.0 KB] || Unassembled_Parts_of_ComPair.webm (4096x2160) [18.2 MB] || Unassembled_Parts_of_ComPair.mp4 (4096x2160) [570.8 MB] || ", "hits": 44 }, { "id": 13873, "url": "https://svs.gsfc.nasa.gov/13873/", "result_type": "Produced Video", "release_date": "2021-07-01T00:00:00-04:00", "title": "Periodic Table of the Elements: Origins of the Elements", "description": "The periodic table organizes all the known elements by atomic number, which is the number of protons in each atom of the element. This version of the table, which draws on data compiled by astronomer Jennifer Johnson from Ohio State University, shows our current understanding of how each element found on Earth was originally produced. Most of them ultimately have cosmic origins. Some elements were created with the birth of the universe, while others were made during the lives or deaths of stars. The Nancy Grace Roman Space Telescope will help us understand the cosmic era when stars first began forming. The mission will help scientists learn more about how elements were created and distributed throughout galaxies.The related Tumblr post is here. || ", "hits": 2225 }, { "id": 13570, "url": "https://svs.gsfc.nasa.gov/13570/", "result_type": "Produced Video", "release_date": "2020-04-27T11:00:00-04:00", "title": "Swift Tracks Water from Interstellar Visitor Borisov", "description": "Watch how NASA’s Neil Gehrels Swift Observatory tracked water production by interstellar comet 2I/Borisov as it sped through the solar system. On average, Borisov produced enough water to fill a standard bathtub in 10 seconds. It shares many traits with solar system comets, which may mean that comets form similarly in different planetary systems.Credit: NASA’s Goddard Space Flight CenterMusic: \"Mesmeric Thoughts\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Swift_Comet_Still.jpg (1920x1080) [599.5 KB] || Swift_Comet_Still_searchweb.png (320x180) [94.6 KB] || Swift_Comet_Still_thm.png (80x40) [6.0 KB] || 13570_Swift_Interstellar_Comet.webm (1920x1080) [17.2 MB] || 13570_Swift_Interstellar_Comet_SRT_Captions.en_US.vtt [2.1 KB] || 13570_Swift_Interstellar_Comet_SRT_Captions.en_US.srt [2.1 KB] || 13570_Swift_Interstellar_Comet_ProRes_1920x1080_2997.mov (1920x1080) [2.1 GB] || 13570_Swift_Interstellar_Comet_Best_1080.mp4 (1920x1080) [375.4 MB] || 13570_Swift_Interstellar_Comet.mp4 (1920x1080) [159.3 MB] || ", "hits": 56 }, { "id": 13076, "url": "https://svs.gsfc.nasa.gov/13076/", "result_type": "Produced Video", "release_date": "2018-09-24T16:00:00-04:00", "title": "Grand Challenge-Cusp Graphics", "description": "GraphicNorth of Norway over the Norwegian and Greenland Seas, a magnetic bubble, known as the cusp, surrounds Earth and dips inward, allowing space particles to funnel in toward the planet.Credit: Andøya Space Center/Trond Abrahamsen || asc-earth-magnetosphere-to-scale_print.jpg (1024x619) [138.1 KB] || asc-earth-magnetosphere-to-scale.jpeg (5352x3240) [13.0 MB] || asc-earth-magnetosphere-to-scale_searchweb.png (320x180) [67.0 KB] || asc-earth-magnetosphere-to-scale_web.png (320x193) [71.7 KB] || asc-earth-magnetosphere-to-scale_thm.png (80x40) [4.3 KB] || ", "hits": 32 }, { "id": 12966, "url": "https://svs.gsfc.nasa.gov/12966/", "result_type": "Produced Video", "release_date": "2018-06-06T00:00:00-04:00", "title": "Measuring the Atmosphere on ATom's Final Flight Around the World", "description": "NASA's Atmospheric Tomography (ATom) mission team just finished their final trip around the world, taking atmospheric samples from all over our home planet. Flying in NASA's DC-8 plane, the scientists and engineers collected their samples during four different trips, one for each season, to see how the atmosphere changed across fall, winter, spring and summer. || ", "hits": 32 }, { "id": 4610, "url": "https://svs.gsfc.nasa.gov/4610/", "result_type": "Visualization", "release_date": "2018-01-19T15:00:00-05:00", "title": "GOLD: Instrument Scanning Coverage", "description": "Visualization of GOLD orbiting Earth with image scanning. This version presents the singly-ionized oxygen density from the IRI model. || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_print.jpg (1024x576) [90.3 KB] || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_searchweb.png (320x180) [79.2 KB] || IRIGOLDscan.GOLDview3_Oion.clockSlate_CRTT.HD1080i.001400_thm.png (80x40) [6.1 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.mp4 (1920x1080) [38.5 MB] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.webm (1920x1080) [10.0 MB] || IRIGOLDscan.GOLDview4_Oion.HD1080i_p30.mp4.hwshow [204 bytes] || ", "hits": 163 }, { "id": 4594, "url": "https://svs.gsfc.nasa.gov/4594/", "result_type": "Visualization", "release_date": "2017-10-31T10:00:00-04:00", "title": "ICON Scans the Ionosphere", "description": "ICON orbits Earth at 575 kilometers altitude, measuring the composition and motions of the ionosphere. || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_print.jpg (1024x576) [105.7 KB] || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_searchweb.png (320x180) [63.8 KB] || IRIDaily.limbwICON_OionHwindIGRF.clockSlate_CRTT.HD1080i.000870_thm.png (80x40) [5.0 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [76.4 MB] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [10.9 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || IRIDaily.limbwICON_OionHwindIGRF.UHD3840_2160p30.mp4 (3840x2160) [217.4 MB] || IRIDaily.limbwICON_OionHwindIGRF.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 85 }, { "id": 4589, "url": "https://svs.gsfc.nasa.gov/4589/", "result_type": "Visualization", "release_date": "2017-10-25T10:00:00-04:00", "title": "Heliophysics Sentinels 2017", "description": "This visualization starts from near Earth and the Earth orbiting satellite fleet out to the Moon, then past the Sun-Earth Lagrange point 1 to out beyond the heliopause. This is the long-play version. || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_print.jpg (1024x576) [136.1 KB] || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_searchweb.png (180x320) [84.6 KB] || Sentinels2017.Sentinels2Voyager.GSE.AU.clockSlate_EarthTarget.UHD3840.00000_thm.png (80x40) [6.0 KB] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.webm (1920x1080) [12.4 MB] || SlowPlay (1920x1080) [0 Item(s)] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.mp4 (1920x1080) [111.6 MB] || SlowPlay (3840x2160) [0 Item(s)] || Sentinels2017.Sentinels2Voyager_2160p30.mp4 (3840x2160) [336.2 MB] || Sentinels2017.Sentinels2Voyager.HD1080i_p30.mp4.hwshow [209 bytes] || ", "hits": 29 }, { "id": 12739, "url": "https://svs.gsfc.nasa.gov/12739/", "result_type": "Produced Video", "release_date": "2017-10-06T10:00:00-04:00", "title": "100 Lunar Days - Parts I and II", "description": "In October 2017, The Lunar Reconnaissance Orbiter celebrates 100 lunar days of being at the Moon. Part 1 of this video series helps explain what a \"lunar day\" is, and what it means for the spacecraft's mission to have been at the Moon for this period of time.Watch this video on the NASA Goddard YouTube channel.Music provided by Killer Tracks: \"Time is Running\" - Dirk Ehlert, Guillermo De La Barreda; \"Buckaroo Instrumental\" - Alan Gold & Fiona Hamilton. || 100LunarDaysTitlecard-PT1_print.jpg (1024x576) [92.7 KB] || 100LunarDaysTitlecard-PT1_searchweb.png (320x180) [55.3 KB] || 100LunarDaysTitlecard-PT1_thm.png (80x40) [6.3 KB] || 100_Lunar_Days-Part1-YouTubeHD.mp4 (1920x1080) [216.9 MB] || 100_Lunar_Days-Part1-MASTER.mov (1920x1080) [1.6 GB] || 100_Lunar_Days-Part1-Facebook.mp4 (1280x720) [181.7 MB] || 100_Lunar_Days-Part1-Twitter.mp4 (1280x720) [32.6 MB] || 100LunarDaysTitlecard-PT1.tif (1920x1080) [9.8 MB] || 100_Lunar_Days-Part1-YouTubeHD.webm (1920x1080) [16.5 MB] || 100LunarDays-Part1-Captions.en_US.srt [2.9 KB] || 100LunarDays-Part1-Captions.en_US.vtt [2.9 KB] || ", "hits": 567 }, { "id": 12731, "url": "https://svs.gsfc.nasa.gov/12731/", "result_type": "Produced Video", "release_date": "2017-10-05T11:00:00-04:00", "title": "Around the World in 11 Research Flights: Behind the Scenes of the ATom Mission", "description": "For the Atmospheric Tomography (ATom) mission, researchers and flight technicians from NASA and its partners are flying around the world, collecting atmospheric samples and studying air quality.This is the the third ATom campaign, studying the atmosphere during autumn in the northern hemisphere. ATom campaigns last a long time -- almost a full month -- and require the researchers and crew to travel the whole time. Rather than work from one static location, the ATom team uses NASA's DC-8 flying laboratory as a home base. Atmospheric scientist Róisín Commane and ATom principal investigator Steven Wofsy gave a look behind the scenes at a month on a research plane. || ", "hits": 20 }, { "id": 12355, "url": "https://svs.gsfc.nasa.gov/12355/", "result_type": "Produced Video", "release_date": "2017-05-18T11:00:00-04:00", "title": "ATom Postcard - Azore Islands to Kangerlussuaq", "description": "Atmospheric scientists Bernadett Weinzierl of the University of Vienna, Paul Newman of Goddard Space Flight Center, and Róisín Commane of Harvard University sent back a video postcard from the last three legs of the Atmospheric Tomography, or ATom mission. Departing Ascension Island in the tropics, the science team traveled up the Atlantic to Terceira Island in the Azores off the coast of Portugal, and then back to the Arctic by way of Kangerlussuaq, Greenland. Finally the team crossed North America to return home to Palmdale, California. || Screen_Shot_2016-08-31_at_11.31.03_AM.png (1911x1072) [1.9 MB] || Screen_Shot_2016-08-31_at_11.31.03_AM_print.jpg (1024x574) [126.6 KB] || Screen_Shot_2016-08-31_at_11.31.03_AM_searchweb.png (320x180) [88.1 KB] || Screen_Shot_2016-08-31_at_11.31.03_AM_thm.png (80x40) [7.1 KB] || ATom_Postcard_-_Azores_to_Kangerlussuaq.webm (1920x1080) [37.1 MB] || ATom_Postcard_-_Azores_to_Kangerlussuaq.en_US.srt [6.6 KB] || ATom_Postcard_-_Azores_to_Kangerlussuaq.en_US.vtt [6.3 KB] || ATom_Postcard_-_Azores_to_Kangerlussuaq.mp4 (1920x1080) [520.1 MB] || ATom_Postcard_-_Azores_to_Kangerlussuaq.mov (1920x1080) [8.8 GB] || ", "hits": 28 }, { "id": 12540, "url": "https://svs.gsfc.nasa.gov/12540/", "result_type": "Produced Video", "release_date": "2017-03-16T00:00:00-04:00", "title": "ATom Postcard - Ascension Island to the Azores Islands", "description": "Atmospheric scientist Róisín Commane of Harvard University sent back a video postcard from Ascension Island and the Azores Islands, the seventh and eighth legs of the Atmospheric Tomography, or ATom mission. Flying over the Atlantic Ocean, the science team saw evidence of fires in Africa and dust from the Sahara.Complete transcript available. || 12540_ATom3_AscensionAzores.00104_print.jpg (1024x576) [127.7 KB] || 12540_ATom3_AscensionAzores.00104_searchweb.png (320x180) [81.7 KB] || 12540_ATom3_AscensionAzores.00104_thm.png (80x40) [5.7 KB] || 12540_ATom3_Ascension_Azores.mp4 (1920x1080) [84.3 MB] || APPLE_TV-12540_ATom3_AscensionAzores_VX-684091_appletv.m4v (1280x720) [44.9 MB] || LARGE_MP4-12540_ATom3_AscensionAzores_VX-684091_large.mp4 (1920x1080) [87.9 MB] || WEBM-12540_ATom3_AscensionAzores_VX-684091.webm (960x540) [33.1 MB] || APPLE_TV-12540_ATom3_AscensionAzores_VX-684091_appletv_subtitles.m4v (1280x720) [44.9 MB] || 12540_ATom3_AscensionAzores.en_US.srt [1.6 KB] || 12540_ATom3_AscensionAzores.en_US.vtt [1.6 KB] || NASA_PODCAST-12540_ATom3_AscensionAzores_VX-684091_ipod_sm.mp4 (320x240) [14.8 MB] || 12540_ATom3_AscensionAzores.mov (1920x1080) [2.2 GB] || NASA_TV-12540_ATom3_AscensionAzores_VX-684091.mpeg (1280x720) [288.0 MB] || PRORES_B-ROLL-12540_ATom3_AscensionAzores_VX-684091_prores.mov (1280x720) [1.1 GB] || YOUTUBE_HQ-12540_ATom3_AscensionAzores_VX-684091_youtube_hq.mov (1920x1080) [288.0 MB] || ", "hits": 39 }, { "id": 12518, "url": "https://svs.gsfc.nasa.gov/12518/", "result_type": "Produced Video", "release_date": "2017-02-17T11:00:00-05:00", "title": "ATom Postcard - Kona, Hawaii", "description": "Atmospheric scientist Jack Dibb of the University of New Hampshire sent a video postcard from the Hawaii leg of the Atmospheric Tomography or ATom mission. On its second worldwide tour, the ATom team flew into Kona, Hawaii, to study small particles like sulfate and nitrate in the atmosphere. Volcanoes like Kilauea, in Hawaii, constantly release sulfate particles, which can oxidize to make sulfuric acid, a component of acid rain. Complete transcript available. || LARGE_MP4-12518_ATom2_Hawaii_large.00007_print.jpg (1024x576) [66.6 KB] || LARGE_MP4-12518_ATom2_Hawaii_large.00007_searchweb.png (320x180) [62.6 KB] || LARGE_MP4-12518_ATom2_Hawaii_large.00007_thm.png (80x40) [4.3 KB] || LARGE_MP4-12518_ATom2_Hawaii_large.mp4 (1920x1080) [91.6 MB] || WEBM-12518_ATom2_Hawaii.webm (960x540) [33.1 MB] || APPLE_TV-12518_ATom2_Hawaii_appletv.m4v (1280x720) [42.7 MB] || APPLE_TV-12518_ATom2_Hawaii_appletv_subtitles.m4v (1280x720) [42.8 MB] || NASA_PODCAST-12518_ATom2_Hawaii_ipod_sm.mp4 (320x240) [17.0 MB] || ATom2_Hawaii.en_US.srt [1.6 KB] || ATom2_Hawaii.en_US.vtt [1.6 KB] || NASA_TV-12518_ATom2_Hawaii.mpeg (1280x720) [299.3 MB] || YOUTUBE_HQ-12518_ATom2_Hawaii_youtube_hq.mov (1920x1080) [252.3 MB] || ", "hits": 24 }, { "id": 12508, "url": "https://svs.gsfc.nasa.gov/12508/", "result_type": "Produced Video", "release_date": "2017-02-09T14:00:00-05:00", "title": "ATom Postcard - Alaska and the Arctic", "description": "On its second worldwide tour, the Atmospheric Tomography (ATom) team starts by surveying the north’s polar regions during winter, which is marked by a build-up of pollution from the United States, Canada, northern China, and Russia. In the spring, sunlight spurs chemical reactions that remove those pollutants and greenhouse gases from the atmosphere.Music credit: Ice Lands by Rik Carter [PRS]Complete transcript available. || LARGE_MP4-12508_ATom1_Alaska_large.00721_print.jpg (1024x576) [120.0 KB] || LARGE_MP4-12508_ATom1_Alaska_large.00721_searchweb.png (320x180) [90.5 KB] || LARGE_MP4-12508_ATom1_Alaska_large.00721_thm.png (80x40) [6.6 KB] || APPLE_TV-12508_ATom1_Alaska_appletv.m4v (1280x720) [22.9 MB] || LARGE_MP4-12508_ATom1_Alaska_large.mp4 (1280x720) [51.1 MB] || WEBM-12508_ATom1_Alaska.webm (960x540) [18.7 MB] || YOUTUBE_HQ-12508_ATom1_Alaska_youtube_hq.mov (1280x720) [78.2 MB] || APPLE_TV-12508_ATom1_Alaska_appletv_subtitles.m4v (1280x720) [22.9 MB] || ATom1_Alaska.en_US.srt [691 bytes] || ATom1_Alaska.en_US.vtt [702 bytes] || NASA_PODCAST-12508_ATom1_Alaska_ipod_sm.mp4 (320x240) [8.1 MB] || NASA_TV-12508_ATom1_Alaska.mpeg (1280x720) [167.8 MB] || ", "hits": 10 }, { "id": 12488, "url": "https://svs.gsfc.nasa.gov/12488/", "result_type": "B-Roll", "release_date": "2017-01-31T12:00:00-05:00", "title": "ATom B-Roll", "description": "The Atmospheric Tomography (ATom) mission takes flight through Earth's atmosphere to understand how short-lived greenhouse gases like ozone and methane contribute to climate change. A suite of instruments aboard NASA's DC-8 flying laboratory will be taking measurements as the science team flies down the Pacific Ocean from Alaska to the southern tip of South America, then north up the Atlantic to Greenland to measure more than 200 gases and particles in the air and their interactions around the world. B-roll available here is from the July 28, 2016, science flight from to the equator and back from Palmdale, California.For more information: NASA Airborne Study Surveys Greenhouse Gases in World Tour: https://www.nasa.gov/feature/goddard/2016/nasa-airborne-study-surveys-greenhouse-gases-in-world-tourNASA Airborne mission Chases Air Pollution Through the Seasons: https://www.nasa.gov/feature/goddard/2017/nasa-airborne-mission-chases-air-pollution-through-the-seasons || ", "hits": 56 }, { "id": 4539, "url": "https://svs.gsfc.nasa.gov/4539/", "result_type": "Visualization", "release_date": "2017-01-13T10:00:00-05:00", "title": "Exploring Earth's Ionosphere: Limb view with approach", "description": "Oxygen ion enhancements at 350km altitude, ionospheric winds at altitudes of 100 km (white) and 350 km (violet) and the low-latitude geomagnetic field. || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_print.jpg (1024x576) [92.1 KB] || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_searchweb.png (320x180) [58.1 KB] || IRIDaily.zoom2limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000400_thm.png (80x40) [4.9 KB] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [89.8 MB] || OionHwindIGRF (1920x1080) [0 Item(s)] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [8.6 MB] || OionHwindIGRF (3840x2160) [0 Item(s)] || IRIDaily.zoom2limb_OionHwindIGRF.2160p30.mp4 (3840x2160) [274.0 MB] || IRIDaily.zoom2limb_OionHwindIGRF.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 57 }, { "id": 4540, "url": "https://svs.gsfc.nasa.gov/4540/", "result_type": "Visualization", "release_date": "2017-01-13T10:00:00-05:00", "title": "Exploring Earth's Ionosphere: Limb view", "description": "This visualization presents data on the concentration of the singly-ionized oxygen atom (rainbow color table, red is highest concentration), the low-latitude geomagnetic field (gold field lines) and the ionospheric winds at two altitude levels, 100km (white) and 350 km (violet). || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_print.jpg (1024x576) [101.4 KB] || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_thm.png (80x40) [5.0 KB] || IRIDaily.limb_OionHwindIGRF.clockSlate_CRTT.HD1080i.000750_searchweb.png (320x180) [62.5 KB] || IRIDaily.limb_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [88.3 MB] || OionHwindIGRF (1920x1080) [0 Item(s)] || OionHwindIGRF (3840x2160) [0 Item(s)] || IRIDaily.limb_OionHwindIGRF.2160p30.webm (3840x2160) [12.4 MB] || IRIDaily.limb_OionHwindIGRF.2160p30.mp4 (3840x2160) [274.0 MB] || IRIDaily.limb_OionHwindIGRF.HD1080i_p30.mp4.hwshow [205 bytes] || ", "hits": 62 }, { "id": 4527, "url": "https://svs.gsfc.nasa.gov/4527/", "result_type": "Visualization", "release_date": "2016-12-14T14:00:00-05:00", "title": "ICON and GOLD: Instrument Scanning Coverage", "description": "Visualization of ICON and GOLD orbiting Earth with image scanning. This version presents several geospace models, including the singly-ionized oxygen density, the low-latitude geomagnetic field, and the high-altitude winds (100km and 350km altitudes). || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_print.jpg (1024x576) [130.5 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_searchweb.png (320x180) [85.0 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.clockSlate_CRTT.UHD3840.001140_thm.png (80x40) [5.9 KB] || IRIGOLDscan.GOLDview3_OionHwindIGRF.HD1080i_p30.mp4 (1920x1080) [82.0 MB] || IRIGOLDscan.GOLDview3_OionHwindIGRF (1920x1080) [0 Item(s)] || IRIGOLDscan.GOLDview3_OionHwindIGRF.HD1080i_p30.webm (1920x1080) [7.6 MB] || IRIGOLDscan.GOLDview3_OionHwindIGRF (3840x2160) [0 Item(s)] || IRIGOLDscan.GOLDview3_OionHwindIGRF_2160p30.mp4 (3840x2160) [258.1 MB] || ", "hits": 51 }, { "id": 4498, "url": "https://svs.gsfc.nasa.gov/4498/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "ICON and GOLD: Exploring the Interface to Space", "description": "A basic view of the orbits for ICON (Ionospheric Connections Explorer) and GOLD (Global-scale Observations of the Limb and Disk). These missions will conduct measurements of ionospheric composition, ionization, and winds to better understand the connection between space weather and its terrestrial impacts.In this visualization, we present GOLD (in geostationary orbit around Earth) and ICON (in low Earth orbit). The colors over Earth represent model data from the IRI (International Reference Ionosphere) model of the density of the singly-ionized oxygen atom at an altitude of 350 kilometers. Red represents high density. The ion density is enhanced above and below the geomagnetic equator (not perfectly aligned with the geographic equator) on the dayside due to the ionizing effects of solar ultraviolet radiation combined with the effects of high-altitude winds and the geomagnetic field. || ", "hits": 30 }, { "id": 4503, "url": "https://svs.gsfc.nasa.gov/4503/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "Exploring the Ionosphere: The View from GOLD", "description": "Closeup view of Earth from the perspective of the GOLD instrument. This version interpolates the IRI model to a higher time cadence for a smoother animation. || IRIDaily.GOLDview_O+ion_O+ionSlice.clockSlate_CRTT.UHD3840.001002_print.jpg (1024x576) [50.7 KB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp.HD1080i_p30.mp4 (1920x1080) [56.7 MB] || IRI.interpolate (1920x1080) [0 Item(s)] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp.HD1080i_p30.webm (1920x1080) [17.1 MB] || IRI.interpolate (3840x2160) [0 Item(s)] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_4503.key [57.9 MB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_4503.pptx [57.6 MB] || IRIDaily.GOLDview_O+ion_O+ionSlice.IRIinterp_2160p30.mp4 (3840x2160) [200.2 MB] || ", "hits": 48 }, { "id": 4504, "url": "https://svs.gsfc.nasa.gov/4504/", "result_type": "Visualization", "release_date": "2016-10-27T14:00:00-04:00", "title": "Exploring the Ionosphere: The Dayside Ionosphere", "description": "A view of the singly-ionizing oxygen atom on the dayside of Earth. This represents the variation of the enhancments due to variation in the geomagnetic field. This version interpolates the IRI model to a higher time cadence for a smoother animation. || IRIDaily.sunward_O+ion.clockSlate_CRTT.UHD3840.001001_print.jpg (1024x576) [58.1 KB] || IRIDaily.sunward_O+ion.IRIinterp.HD1080i_p30.mp4 (1920x1080) [50.1 MB] || IRI.interpolated (1920x1080) [0 Item(s)] || IRIDaily.sunward_O+ion.IRIinterp.HD1080i_p30.webm (1920x1080) [17.1 MB] || IRIDaily.sunward_O+ion.IRIinterp.UHD3840_2160p30.mp4 (3840x2160) [72.7 MB] || IRI.interpolated (3840x2160) [0 Item(s)] || IRIDaily.sunward_O+ion.IRIinterp_4504.key [51.9 MB] || IRIDaily.sunward_O+ion.IRIinterp_4504.pptx [51.6 MB] || exploring-the-ionosphere-the-dayside-ionosphere.hwshow [308 bytes] || ", "hits": 39 }, { "id": 12354, "url": "https://svs.gsfc.nasa.gov/12354/", "result_type": "Produced Video", "release_date": "2016-08-29T22:00:00-04:00", "title": "ATom Postcard - Punta Arenas to Ascension Island", "description": "Postcard #3Atmospheric scientist Róisín Commane and Principal Investigator Steven Wofsy both of Harvard University sent back a video postcard from the Atlantic legs of the Atmospheric Tomography, or ATom mission. The science team left Christchurch New Zealand and traveled past Antarctica to Punta Arenas, Chile at the bottom of the world. Then they went up the Atlantic Ocean to Ascension Island, just south of the equator. || Screen_Shot_2016-08-29_at_2.44.38_AM_print.jpg (1024x574) [143.5 KB] || Screen_Shot_2016-08-29_at_2.44.38_AM.png (2154x1209) [3.4 MB] || Screen_Shot_2016-08-29_at_2.44.38_AM_searchweb.png (320x180) [98.6 KB] || Screen_Shot_2016-08-29_at_2.44.38_AM_thm.png (80x40) [7.1 KB] || ATom_Postcard_3_-_Punta_Arenas_to_Ascension.webm (1920x1080) [23.2 MB] || ATom_Postcard_3_-_Punta_Arenas_to_Ascension.en_US.srt [4.2 KB] || ATom_Postcard_3_-_Punta_Arenas_to_Ascension.en_US.vtt [4.0 KB] || ATom_Postcard_3_-_Punta_Arenas_to_Ascension.mov (1920x1080) [5.5 GB] || ", "hits": 20 }, { "id": 12350, "url": "https://svs.gsfc.nasa.gov/12350/", "result_type": "Produced Video", "release_date": "2016-08-29T11:00:00-04:00", "title": "ATom Mission interview clips", "description": "The ATom mission aboard NASA's DC-8 flying laboratory is sampling world-wide in one of the most extensive surveys of the atmosphere to date, measuring over 200 gases as well as airborne particles. The science team is particularly interested in methane, tropospheric ozone and black carbon particles, which have strong effects on climate and which all have both human and natural origins.Below are interviews with four scientists participating in the research flights:* Donald Blake, UC Irvine* Róisín Commane, Harvard University* Tom Ryerson, NOAA* Jack Dibbs, University of New HampshireFollow along with all eight of our #EarthExpeditions here: http://www.nasa.gov/earthexpeditions || ", "hits": 16 }, { "id": 12342, "url": "https://svs.gsfc.nasa.gov/12342/", "result_type": "Produced Video", "release_date": "2016-08-16T18:00:00-04:00", "title": "ATom Postcard - Samoa to New Zealand", "description": "Principal Investigator Steven Wofsy of Harvard University and atmospheric scientist Paul Newman of NASA’s Goddard Space Flight Center sent back a video postcard of the second two legs of the Atmospheric Tomography, or ATom mission. They and the science team traversed the tropical Pacific from Kona, Hawaii to Pago Pago, American Samoa, and then to Christchurch, New Zealand. || Screen_Shot_2016-08-16_at_6.11.17_PM_print.jpg (1024x574) [203.0 KB] || Screen_Shot_2016-08-16_at_6.11.17_PM.png (2305x1293) [4.5 MB] || Screen_Shot_2016-08-16_at_6.11.17_PM_searchweb.png (320x180) [124.7 KB] || Screen_Shot_2016-08-16_at_6.11.17_PM_thm.png (80x40) [8.3 KB] || Samoa_to_New_Zealand.webm (1280x720) [24.5 MB] || Samoa_to_New_Zealand.en_US.srt [4.7 KB] || Samoa_to_New_Zealand.en_US.vtt [4.5 KB] || Samoa_to_New_Zealand.mp4 (1280x720) [245.1 MB] || Samoa_to_New_Zeland.mov (1280x720) [3.1 GB] || ", "hits": 23 }, { "id": 12337, "url": "https://svs.gsfc.nasa.gov/12337/", "result_type": "Produced Video", "release_date": "2016-08-10T15:00:00-04:00", "title": "ATom Mission Postcard - Palmdale to Kona", "description": "Principal Investigator Steven Wofsy of Harvard University and atomsperhic scientist Paul Newman of NASA’s Goddard Space Flight Center sent back a video postcard of the first two legs of the Atmospheric Tomography, or ATom mission. The science team first traveled from Palmdale California to Anchorage Alaksa by way of the North Pole, and one their second leg flew south to Kona, Hawaii. || Screen_Shot_2016-08-10_at_3.27.23_PM.png (1911x1069) [3.1 MB] || Screen_Shot_2016-08-10_at_3.27.23_PM_print.jpg (1024x572) [177.1 KB] || Screen_Shot_2016-08-10_at_3.27.23_PM_searchweb.png (320x180) [111.1 KB] || Screen_Shot_2016-08-10_at_3.27.23_PM_thm.png (80x40) [7.7 KB] || ATom_Final.webm (1920x1080) [19.0 MB] || Atom_Final.en_US.srt [3.4 KB] || Atom_Final.en_US.vtt [3.2 KB] || ATom_Final.mov (1920x1080) [4.6 GB] || ATom_Final.mp4 (1920x1080) [170.2 MB] || ", "hits": 31 }, { "id": 4322, "url": "https://svs.gsfc.nasa.gov/4322/", "result_type": "Visualization", "release_date": "2015-06-24T00:00:00-04:00", "title": "The Multiple CMEs of June, 2015", "description": "A view of multiple CMEs which erupted from the Sun in the latter half of June 2015. Their trajectories, and potential impacts on Earth and space assets, are propagated with the Enlil model. || 2015June20_high2AU.full.0006_print.jpg (1024x576) [48.8 KB] || 2015June20_high2AU.full.0006_searchweb.png (320x180) [38.5 KB] || 2015June20_high2AU.full.0006_thm.png (80x40) [4.7 KB] || 2015June20_high2AU.full.HD1080.webm (1920x1080) [406.6 KB] || 2015June20_high2AU.full.HD1080.mov (1920x1080) [1.8 MB] || 1920x1080_16x9_10p (1920x1080) [4.0 KB] || ", "hits": 38 }, { "id": 4288, "url": "https://svs.gsfc.nasa.gov/4288/", "result_type": "Visualization", "release_date": "2015-06-10T00:00:00-04:00", "title": "The 2015 Earth-Orbiting Heliophysics Fleet", "description": "Movie showing the heliosphysics missions from near Earth orbit out to the orbit of the Moon.This video is also available on our YouTube channel. || Helio2015A.MMStour.slate_RigRHS.HD1080i.0500_print.jpg (1024x576) [112.6 KB] || Helio2015A.MMStour.HD1080.webm (1920x1080) [6.7 MB] || WithoutTimeStamp (1920x1080) [128.0 KB] || Helio2015A.MMStour.HD1080.mov (1920x1080) [196.3 MB] || Helio2015_4288.pptx [198.6 MB] || Helio2015_4288.key [201.3 MB] || ", "hits": 47 }, { "id": 12561, "url": "https://svs.gsfc.nasa.gov/12561/", "result_type": "Produced Video", "release_date": "2014-12-16T10:00:00-05:00", "title": "Possible Methane Sources and Sinks on Mars", "description": "There are several possible ways that methane can be created, stored, and released on Mars, including both biological and non-biological pathways. || Mars_Methane_Sources_Sinks_PIA19088.jpg (1440x1080) [227.6 KB] || Mars_Methane_Sources_Sinks_PIA19088_searchweb.png (320x180) [108.1 KB] || Mars_Methane_Sources_Sinks_PIA19088_thm.png (80x40) [6.9 KB] || Mars_Methane_Sources_Sinks_PIA19088.tif (1440x1080) [4.5 MB] || ", "hits": 209 }, { "id": 11613, "url": "https://svs.gsfc.nasa.gov/11613/", "result_type": "Produced Video", "release_date": "2014-08-01T10:00:00-04:00", "title": "EUNIS Sees Evidence for Nanoflare Heating", "description": "Scientists have recently gathered some of the strongest evidence to date to explain what makes the sun's outer atmosphere so much hotter than its surface. The new observations show temperatures in the atmosphere so hot that only one current theory explains them: something called nanoflares – a constant peppering of impulsive bursts of heating, none of which can be individually detected — provide the mysterious extra heat. These new observations come from just six minutes worth of data from one of NASA's least expensive type of missions, a sounding rocket. The EUNIS mission, short for Extreme Ultraviolet Normal Incidence Spectrograph, launched on April 23, 2013, gathering a new snapshot of data every 1.3 seconds to track the properties of material over a wide range of temperatures in the complex solar atmosphere. The unique capabilities of EUNIS enabled researchers to obtain these results. The spectrograph was able to clearly and unambiguously distinguish the observations representing the extremely hot material – emission lines showing light with a wavelength of 592.6 angstrom, where an angstrom is the size of an atom — from a very nearby light wavelength of 592.2 angstroms. || ", "hits": 43 }, { "id": 11550, "url": "https://svs.gsfc.nasa.gov/11550/", "result_type": "Produced Video", "release_date": "2014-07-28T13:00:00-04:00", "title": "NASA X-ray Instrument Confirms the 'Local Hot Bubble'", "description": "New findings from the NASA-funded Diffuse X-ray emission from the Local Galaxy (DXL) mission have resolved a decades-old puzzle about a fog of low-energy X-rays observed over the entire sky. Using refurbished detectors first flown on a NASA sounding rocket in the 1970s, astronomers have now confirmed the long-held suspicion that much of this glow stems from a region of million-degree interstellar plasma known as the local hot bubble, or LHB.In the 1990s, a six-month all-sky survey by the German X-ray observatory ROSAT provided improved maps of the soft X-ray diffuse background. But it also revealed that comets were an unexpected source of soft X-rays. As scientists began to understand this process, called solar wind charge exchange, they realized it could occur anywhere neutral atoms interacted with the solar wind, leading scientists to challenge the LHB interpretation.On Dec. 12, 2012, DXL launched from White Sands Missile Range in New Mexico atop a NASA Black Brant IX sounding rocket, reaching a peak altitude of 160 miles (258 km) and spending five minutes above Earth's atmosphere. The mission design allowed the instrument to observe a worst-case scenario involving charge exchange with interstellar gas.The solar system is currently passing through a small cloud of cold interstellar gas as it moves through the galaxy. The cloud’s neutral hydrogen and helium atoms stream through the planetary system at about 56,000 mph (90,000 km/h). While hydrogen atoms quickly ionize and respond to numerous forces, the helium atoms travel paths largely governed by the sun's gravity. This creates a \"helium focusing cone\" downstream from the sun that crosses Earth's orbit and is located high in the sky near midnight in early December. Better still, it forms a region with a much greater density of neutral atoms and a correspondingly enhanced charge exchange rate.The solar wind originates in the sun's corona, the hottest part of its atmosphere, so its atoms have been ionized, stripped of many of their electrons. When these particles collide with a neutral atom, one of its electrons often jumps to the solar wind ion. Once captured, the electron briefly remains in an excited state, then emits a soft X-ray and settles down at a lower energy. To establish a baseline for the soft X-ray background, the researchers used data captured by the ROSAT mission in September 1990 in a direction looking along, rather than into, the helium focusing cone. The results indicate that only about 40 percent of the soft X-ray background originates within the solar system, which means the LHB is the dominant source. || ", "hits": 122 }, { "id": 4167, "url": "https://svs.gsfc.nasa.gov/4167/", "result_type": "Visualization", "release_date": "2014-07-23T00:00:00-04:00", "title": "The Big CME that Missed Earth", "description": "July of 2012 witnessed the eruption of a very large and fast solar coronal mass ejection (CME) (see NASA STEREO Observes One of the Fastest CMEs On Record and Carrington-class CME Narrowly Misses Earth ). While not directed at Earth, it was sufficiently large that it could have seriously disrupted the global electrical infrastructure. The event did impact STEREO-A of NASA's heliophysics fleet which provided a host of measurements (see Sentinels of the Heliosphere).One of the conditions which contributed to the high speed of this event is that two smaller CMEs were launched a little earlier, and these events cleared out much of the solar wind material, leaving little to slow the outflow of the July 23 event (UTC).In the visualizations below, generated from the Enlil space weather model, green represents particle density, usually protons and other ions. In green, we see the Parker spiral moving out from the sun generated by the sun's current sheet (Wikipedia). Red represents particles at high temperatures and shows the CME is hotter than the usual solar wind flow. Large changes in density are represented in blue. These three colors sometimes combine to tell us more about the characteristics of the event (noted in the 3-color Venn diagram below).However, if this CME had struck Earth's magnetosphere, which has a much stronger magnetic field, the changing magnetic field would induce much larger voltages in systems with long electrical conductors, such as power lines that run over long distances. These significantly higher voltages can damage power transformers. || ", "hits": 162 }, { "id": 11479, "url": "https://svs.gsfc.nasa.gov/11479/", "result_type": "Produced Video", "release_date": "2014-04-24T00:00:00-04:00", "title": "Cold Atom Lab", "description": "Matter conceals a squiggly alter ego. While everyone knows matter’s everyday particle persona, it also has hidden wave properties, akin to sound or light. To explore these properties, scientists chill atoms to the max—or very close to it. As temperatures plummet to nearly absolute zero (-459.67°F), atoms start looking more like waves and less like particles. Droves of atomic wavelets can even start tuning in to the same frequency and wiggle as a single, coherent wave in what’s called a Bose-Einstein condensate. On Earth, gravity’s incessant tug makes it difficult to keep atoms trapped in a condensed state for long. But in 2016, researchers will be able to keep matter colder for longer in the microgravity environment of NASA’s Cold Atom Lab aboard the International Space Station. Watch the video to learn more about this exceedingly cool mission. || ", "hits": 120 }, { "id": 4127, "url": "https://svs.gsfc.nasa.gov/4127/", "result_type": "Visualization", "release_date": "2013-12-16T12:00:00-05:00", "title": "The 2013 Earth-Orbiting Heliophysics Fleet", "description": "There've been a few changes since the 2012 Earth-Orbiting Heliophysics Fleet. As of Fall of 2013, here's a tour of the NASA Near-Earth Heliophysics fleet, covering the space from near-Earth orbit out to the orbit of the Moon.The satellite orbits are color coded for their observing program:Magenta: TIM (Thermosphere, Ionosphere, Mesosphere) observationsYellow: solar observations and imageryCyan: Geospace and magnetosphereViolet: Heliospheric observationsNear-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 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. SORCE: Monitors solar intensity across a broad range of the electromagnetic spectrum.AIM: Images and measures noctilucent clouds. SVS pageVan Allen Probes: Two probes moving along the same orbit esigned to study the impact of space weather on Earth's radiation belts. SVS pageTWINS: Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) are two probes observing the Earth with neutral atom imagers.IRIS: Interface Region Imaging Spectrograph is designed to take high-resolution spectra and images of the region between the solar photosphere and solar atmosphere.Geosynchronous Fleet:SDO: Solar Dynamics Observatory keeps the Sun under continuous observation at 16 megapixel resolution.GOES: The newest GOES satellites include a solar X-ray imager operated by NOAA.Geospace 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 three satellites to study how magnetospheric instabilities produce substorms. Two of the original five satellites were moved into lunar orbit to become ARTEMIS. SVS page IBEX: The Interstellar Boundary Explorer measures the flux of neutral atoms from the heliopause.Lunar Orbiting FleetARTEMIS: Two of the THEMIS satellites were moved into lunar orbit to study the interaction of the Earth's magnetosphere with the Moon. || ", "hits": 40 }, { "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": 22 }, { "id": 4087, "url": "https://svs.gsfc.nasa.gov/4087/", "result_type": "Visualization", "release_date": "2013-07-10T13:00:00-04:00", "title": "IBEX Heliotail Observations", "description": "The IBEX (Interstellar Boundary EXplorer) continues to collect data on the flux of neutral atoms from the boundary of the solar wind with the interstellar medium.Starting with the IBEX satellite in orbit around the Earth, we zoom out to beyond the orbit of Neptune, illustrating the direction of the Sun relative to the local stars (red arrow) and relative to the local interstellar medium (violet arrow). These directions are different because the local interstellar medium (mostly gas and dust) move relative to the local stars.The boundaries of the termination shock (red ellipsoidal surface) and heliopause (green) created by the interaction of the solar wind with the interstellar medium is displayed. The camera rotates to a view 'nose on' with the heliopause, and a sphere is faded in representing the region where the neutral atoms detected by IBEX originate. The sphere around the Sun is 'unwrapped' to reproject the IBEX data into an approximately Aitoff projection. || ", "hits": 70 }, { "id": 11301, "url": "https://svs.gsfc.nasa.gov/11301/", "result_type": "Produced Video", "release_date": "2013-07-10T12:30:00-04:00", "title": "IBEX Provides First View Of the Solar System’s Tail", "description": "This page contains resources from the July 10, 2013 media briefing.To watch the media briefing on YouTube, click here.To view the web short on YouTube about this story, click here.NASA’s Interstellar Boundary Explorer, or IBEX, recently mapped the boundaries of the solar system’s tail, called the heliotail. By combining observations from the first three years of IBEX imagery, scientists have mapped out a tail that shows a combination of fast and slow moving particles. The entire structure twisted, because it experiences the pushing and pulling of magnetic fields outside the solar system. || ", "hits": 55 }, { "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": 64 }, { "id": 4078, "url": "https://svs.gsfc.nasa.gov/4078/", "result_type": "Visualization", "release_date": "2013-05-16T00:00:00-04:00", "title": "CMEpalooza - May 15, 2013", "description": "Active Region 11748 launches another big coronal mass ejection (CME) into the solar system along with X-class flares. See CMEpalooza - May 14, 2013 for the previous event. This is the forecast trajectory from the Community-Coordinated Modeling Center of the CME through the inner solar system. || ", "hits": 15 }, { "id": 4079, "url": "https://svs.gsfc.nasa.gov/4079/", "result_type": "Visualization", "release_date": "2013-05-16T00:00:00-04:00", "title": "CMEpalooza - May 14, 2013", "description": "As active Region 11748 rotated into Earth's view over the left limb of the sun it erupted with many large flares and coronal mass ejections (CMEs). Some of the flares were X-class.This event is of particular interest as it launched three CMEs that are expected to merge into a large plasma cloud and continue heading out into the solar system. A few NASA spacecraft were in the path of this event — their operators can put the spacecraft into safe mode for protection when required. || ", "hits": 45 }, { "id": 4064, "url": "https://svs.gsfc.nasa.gov/4064/", "result_type": "Visualization", "release_date": "2013-04-12T12:00:00-04:00", "title": "The CME of April 11, 2013", "description": "The CME launched from the Sun on April 11, 2013 was modelled at the Community-Coordinated Modeling Center (CCMC) at NASA's Goddard Space Flight Center. These model runs are used for testing various space weather models and for protecting NASA assets (spacecraft AND astronauts) throughout the Solar System.Different colors of a red, green, blue color palette are used to designate different physical variables from the simulation. When the three colors combine, they create a dramatic example of how the coronal mass ejection (CME) is different from the solar wind. || ", "hits": 22 }, { "id": 4058, "url": "https://svs.gsfc.nasa.gov/4058/", "result_type": "Visualization", "release_date": "2013-03-27T00:00:00-04:00", "title": "Space Weather @ Mars: The CME of March 5, 2013", "description": "These images were produced from a space weather model known as ENLIL named after the Sumerian storm god. It shows the way a coronal mass ejection (CME) on March 5, 2013, was expected to travel. The view on the left is top down, while the one on the right shows Earth from the side.To protect their space assets from excessive radiation, NASA and other organizations research the fundamental processes behind space weather such as CMEs, integrating them into research models, which are run continuously at the Community-Coordinated Modeling Center (CCMC) at NASA Goddard.When CMEs occur on the sun, models are generated with the best event information available at the time and propagated forward to estimate regions in the solar system that might be affected. The models take about an hour or two to run. The CMEs themselves usually take one or two days to reach other planets or spacecraft.The March 5 CME moved towards Mars and the STEREO-B spacecraft (blue spacecraft icon). This allowed mission operators to take steps to protect STEREO-B as well as spacecraft operating around and on Mars. || ", "hits": 47 }, { "id": 4057, "url": "https://svs.gsfc.nasa.gov/4057/", "result_type": "Visualization", "release_date": "2013-03-25T00:00:00-04:00", "title": "LEND Looks for Water at the South Pole", "description": "Since Lunar Reconnaissance Orbiter (LRO) entered lunar orbit in 2009, its neutron detector, LEND, has been counting the neutrons coming from the Moon's surface.Neutrons are created when galactic cosmic rays strike atoms in the lunar regolith. These neutrons bounce from atom to atom like billiard balls, losing energy with each collision. Along the way, some of these neutrons escape into space, where LEND can detect them.The presence of hydrogen in the lunar soil reduces the number of neutrons that escape. To map out likely deposits of water ice, LEND scientists look for this deficit of neutrons in the epithermal (medium) energy range.If the deficit were simply due to random fluctuations, the hydrogen map would never coalesce into a sharp image, but as this animation shows, the map of epithermal neutron deficit at the south pole of the Moon improves over time and converges on particular spots. These include especially strong signals in the permanently shadowed parts of Cabeus and Shoemaker craters, where ice would be completely shielded from the sun. But LEND and other missions have found signs of water in places that aren't permanently shadowed while apparently excluding some places that are, both of which are surprising and exciting discoveries. || ", "hits": 183 }, { "id": 4056, "url": "https://svs.gsfc.nasa.gov/4056/", "result_type": "Visualization", "release_date": "2013-03-18T00:00:00-04:00", "title": "The CME of March 15, 2013", "description": "The CME launched from the Sun on March 15, 2013 was modelled at the Community-Coordinated Modeling Center (CCMC) at NASA's Goddard Space Flight Center. These model runs are used for testing various space weather models and for protecting NASA assets (spacecraft AND astronauts) throughout the Solar System.Different colors of a red, green, blue color palette are used to designate different physical variables from the simulation. When the three colors combine, they create a dramatic example of how the coronal mass ejection (CME) is different from the solar wind. || ", "hits": 53 }, { "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": 687 }, { "id": 4010, "url": "https://svs.gsfc.nasa.gov/4010/", "result_type": "Visualization", "release_date": "2012-12-20T09:00:00-05:00", "title": "Space Weather Research: The CME of March 2012", "description": "Forecasting space weather is of vital importance in protecting NASA assets around the solar system. For this reason, NASA routinely tests various space weather models at the Community-Coordinated Modeling Center (CCMC).This visualization is constructed from a computer model run of a coronal mass ejection (CME) launched from the sun in early March, 2012. The preliminary CME parameters were measured from instruments on the STEREO (the red and blue satellite icons) and SDO (in Earth orbit) satellites. The Enlil model was used to propagate those parameters through the solar system. From this model, they can estimate the strength and time of arrival of the CME at various locations around the solar system. This allows other missions to either safe-mode their satellites for protection, or allow them to conduct measurements to test the accuracy of the model. || ", "hits": 49 }, { "id": 11093, "url": "https://svs.gsfc.nasa.gov/11093/", "result_type": "Produced Video", "release_date": "2012-10-11T13:00:00-04:00", "title": "Atomic Interferometry", "description": "Einstein predicted gravity waves in his general theory of relativity, but to date these ripples in the fabric of space-time have never been observed. Now a scientific research technique called Atomic Interferometry is trying to re-write the canon. In conjunction with researchers at Stanford University, scientists at NASA Goddard are developing a system to measure the faint gravitational vibrations generated by movement of massive objects in the universe. The scientific payoff could be important, helping better clarify key issues in our understanding of cosmology. But application payoff could be substantial, too, with the potential to develop profound advances in fields like geolocation and timekeeping. In this video we examine how the system would work, and the scientific underpinnings of the research effort. || ", "hits": 35 }, { "id": 11084, "url": "https://svs.gsfc.nasa.gov/11084/", "result_type": "Produced Video", "release_date": "2012-10-04T00:00:00-04:00", "title": "Origin Of Light", "description": "An elegant interaction powers the sun, producing the light and energy that makes life possible. That interaction is called fusion, and it naturally occurs when two atoms are heated and compressed so intensely that their nuclei merge into a new element. This process often leads to the creation of a photon, the particles of light that are released from the sun. However, before exiting our star, each photon must first undergo a long journey. Over the course of 40,000 years it will be absorbed by other atoms and emitted repeatedly until reaching the sun's surface. Once there, the photons stream out, illuminating Earth, the solar system and beyond. The number released from the surface every second is so vast that it is more than a billion billion times greater than the number of grains of sand on our planet. Watch the animation to see how atoms deep inside the sun's core melt together and generate light. || ", "hits": 2576 }, { "id": 3900, "url": "https://svs.gsfc.nasa.gov/3900/", "result_type": "Visualization", "release_date": "2012-01-31T13:00:00-05:00", "title": "The Local Interstellar Wind as Seen by IBEX", "description": "This visual presents a color-coded full-sky neutral atom map in a Hammer projection. This map is different from earlier IBEX maps in that it shows atoms only at energies where the interstellar wind is the brightest feature in the maps. In Earth's orbit, where IBEX makes its observations, the maximum flow (in red) is seen to arrive from Libra instead of Scorpio because the interstellar wind is forced to curve around the Sun by gravity. || ", "hits": 15 }, { "id": 10905, "url": "https://svs.gsfc.nasa.gov/10905/", "result_type": "Produced Video", "release_date": "2012-01-31T13:00:00-05:00", "title": "Interstellar Neutral Atoms", "description": "Animation of the interstellar interaction with our Sun-one of billions of stars that orbits around the galaxy. As we zoom in through the galaxy we can see our heliosphere; then if we travel along with the interstellar material, we can see how only a very rare few are directed along precisely the right path to make the 30 year, 15 billion mile journey and enter IBEX's low energy sensor and be detected.For press release media associated with this animation, go: here. || ", "hits": 77 }, { "id": 10906, "url": "https://svs.gsfc.nasa.gov/10906/", "result_type": "Produced Video", "release_date": "2012-01-31T13:00:00-05:00", "title": "NASA's IBEX Spacecraft Reveals New Observations of Interstellar Matter", "description": "A great magnetic bubble surrounds the solar system as it cruises through the galaxy. The sun pumps the inside of the bubble full of solar particles that stream out to the edge until they collide with the material that fills the rest of the galaxy, at a complex boundary called the heliosheath. On the other side of the boundary, electrically charged particles from the galactic wind blow by, but rebound off the heliosheath, never to enter the solar system. Neutral particles, on the other hand, are a different story. They saunter across the boundary as if it weren't there, continuing on another 7.5 billion miles for 30 years until they get caught by the sun's gravity, and sling shot around the star. There, NASA's Interstellar Boundary Explorer lies in wait for them. Known as IBEX for short, this spacecraft methodically measures these samples of the mysterious neighborhood beyond our home. IBEX scans the entire sky once a year, and every February, its instruments point in the correct direction to intercept incoming neutral atoms. IBEX counted those atoms in 2009 and 2010 and has now captured the best and most complete glimpse of the material that lies so far outside our own system. The results? It's an alien environment out there: the material in that galactic wind doesn't look like the same stuff our solar system is made of.More than just helping to determine the distribution of elements in the galactic wind, these new measurements give clues about how and where our solar system formed, the forces that physically shape our solar system, and even the history of other stars in the Milky Way.In a series of science papers appearing in the Astrophysics Journal on January 31, 2012, scientists report that for every 20 neon atoms in the galactic wind, there are 74 oxygen atoms. In our own solar system, however, for every 20 neon atoms there are 111 oxygen atoms. That translates to more oxygen in any given slice of the solar system than in the local interstellar space. For media associated with this release, go to #10905 and #3900. || ", "hits": 153 }, { "id": 10823, "url": "https://svs.gsfc.nasa.gov/10823/", "result_type": "Produced Video", "release_date": "2011-09-20T00:00:00-04:00", "title": "Up In The Stratosphere, Ozone Thins Again", "description": "Each spring in the Southern Hemisphere marks the beginning of a precipitous annual decline in ozone levels over Antarctica. The process starts in the dark of Antarctic winter as sub-freezing temperatures give rise to large numbers of wispy, iridescent clouds located high over the continent, 80,000 feet up in a layer of air called the stratosphere. The clouds are key to the depletion of ozone because a cascade of ozone-depleting reactions, fueled by human-generated chlorofluorocarbons, halons and methyl bromide compounds, occur within them. When the sun shines over Antarctica in the spring, its rays release chlorine and bromine atoms from these chemicals in forms that attack ozone. The atoms eat away as much as 70 percent of the ozone layer, creating an \"ozone hole\" to form over the region. So far, the hole appears slightly larger than it was this time last year, but it won't reach its maximum size until mid-October. In the visualization below watch the ozone hole grow from July 1 to September 16, 2011. || ", "hits": 30 }, { "id": 10706, "url": "https://svs.gsfc.nasa.gov/10706/", "result_type": "Produced Video", "release_date": "2011-01-10T16:00:00-05:00", "title": "Terrestrial Gamma-ray Flashes Create Antimatter", "description": "NASA's Fermi Gamma-ray Space Telescope has detected beams of antimatter launched by thunderstorms. Acting like enormous particle accelerators, the storms can emit gamma-ray flashes, called TGFs, and high-energy electrons and positrons. Scientists now think that most TGFs produce particle beams and antimatter.For additional animations showing bremsstrahlung and pair production gamma ray reactions, go here.For more visualizations showing Fermi's TGF detections, go to#3747, #3748, and #3756.For animations of the Fermi spacecraft and matter/antimatter, go to#10707 and #10651. || ", "hits": 273 }, { "id": 10690, "url": "https://svs.gsfc.nasa.gov/10690/", "result_type": "Produced Video", "release_date": "2010-11-09T13:00:00-05:00", "title": "How to make a gamma ray", "description": "A series of animations showing how gamma rays can be created through various particle interactions. || ", "hits": 362 }, { "id": 3769, "url": "https://svs.gsfc.nasa.gov/3769/", "result_type": "Visualization", "release_date": "2010-09-30T12:00:00-04:00", "title": "IBEX Skymaps and the Bright Stars", "description": "In this image set, the brighter stars from the Tycho skymap have been reprojected into positions corresponding to the coordinate system used by the IBEX mission.The colors represent the number of neutral atoms (in the specified band of energies) detected by IBEX in each block of sky. Each block in the map is roughly a square about 6 degrees by 6 degrees (or the width of 12 full Moons, on a side). For the energy band displayed of 2.73 keV, violet corresponds to undetectable emission, while red corresponds to the detection of about 50 atoms per second per square centimeter in the angular segment of the sky. There is a 'hole' in the data (black) created when the IBEX scan cuts through the Earth's magnetotail.The images in this set have been co-registered for easy compositing. || ", "hits": 28 }, { "id": 3770, "url": "https://svs.gsfc.nasa.gov/3770/", "result_type": "Visualization", "release_date": "2010-09-30T12:00:00-04:00", "title": "IBEX Observes Changes in Heliopause Emission", "description": "The camera view moves from the heliosphere 'nose', the apparent direction of the heliopause relative to the interstellar wind, towards the 'knot'. The 'knot' represents a direction of high emission of neutral atoms which has changed significantly in the six months since the first IBEX map.We fade-in an artistic conception of the 'knot', which untangles during the six months as we fade to the second IBEX map. || ", "hits": 11 }, { "id": 3740, "url": "https://svs.gsfc.nasa.gov/3740/", "result_type": "Visualization", "release_date": "2010-07-08T00:00:00-04:00", "title": "Space Weather Event: The View from L1", "description": "We start from a position 'behind' the Earth, looking towards the Sun. From this position we see the orbit of the Moon as well as three of the heliospheric 'sentinels' (see \"Sentinels of the Heliosphere\"), ACE, SOHO, and Wind patrolling along 'halo orbits' (Wikipedia) around the Sun-Earth Lagrange Point, L1.The CME (orange isosurface) erupts, heading towards the Earth. The density enhancement of the CME is visible in slice of data in the Earth's orbit plane which provides a better sense of when the CME actually reaches the Earth.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red), 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and make it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 31 }, { "id": 3743, "url": "https://svs.gsfc.nasa.gov/3743/", "result_type": "Visualization", "release_date": "2010-07-08T00:00:00-04:00", "title": "Space Weather Event: Close-up on the Earth Environment", "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth and move into a position above the Earth's orbital plane with the Earth (geospace) environment in view.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors are: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, the dominant component of the solar wind.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 39 }, { "id": 3739, "url": "https://svs.gsfc.nasa.gov/3739/", "result_type": "Visualization", "release_date": "2010-07-06T00:00:00-04:00", "title": "Space Weather Event: Incoming View", "description": "We open with a view from high above the ecliptic plane, at the space between the Sun (left) and the Earth (within the small rectangular box on the right). In the plane of the Earth's orbit, we show a 'slice' of the Enlil model showing the particle density profile of the solar wind (white to yellow for decreasing particle density). The spiral 'rotating water sprinkler' pattern in the density is the Parker spiral (Wikipedia). The nested grid pattern centered on the Earth, provides a sense of scale to the scene. The smallest grid square in the opening view is 1,000 Earth radii on each side. The scale changes by a factor of ten for each step larger or smaller in size.We zoom down to the Earth as the CME (orange surface) erupts in the direction of the Earth, then move into a position behind the Earth with the Sun visible in the distance.As the particle density enhancement from the CME strikes the Earth, we see the Earth's magnetosphere respond, with the outer, high density surface (red) 'blown away'. This surface location corresponds roughly to the location of the bow shock. The bow shock has not been eliminated, only some of its particles have been depleted, to be carried off in the CME and solar wind. As the densest material of the CME passes (orange surface), plasma from the CME continues to flow by the Earth, stretching the magnetosphere into a long, thin structure behind the Earth.The magnetosphere slowly recovers from the 'impact', and regions that can confine higher particle densities reform - the red surfaces return. But not for long as the rarefaction (Wikipedia) behind the CME reaches the Earth. This lower density region provides fewer particles to repopulate the magnetosphere and makes it easier for particles confined in the magnetosphere to 'leak' out into the solar wind.For the BATS-R-US model, the isosurface colors correpond to densities of: red=20 AMUs per cubic centimeter, yellow=10.0 AMUs per cubic centimeter, light blue=1.0 AMUs per cubic centimeter, and blue=0.1 AMUs per cubic centimeter. An AMU corresponds to about the mass of a hydrogen atom, so the value roughly corresponds to the number of atoms per cubic centimeter.This visualization is part of a series of visualizations on space weather modeling. || ", "hits": 18 }, { "id": 3635, "url": "https://svs.gsfc.nasa.gov/3635/", "result_type": "Visualization", "release_date": "2009-10-15T12:00:00-04:00", "title": "IBEX First Skymap Release", "description": "The Interstellar Boundary Explorer (IBEX) mission science team has used data from NASA's IBEX spacecraft to construct the first-ever all-sky map of the interactions occurring at the edge of the solar system, where the sun's influence diminishes and interacts with the interstellar medium. The interstellar boundary region shields our solar system from most of the dangerous galactic cosmic radiation that would otherwise enter from interstellar space.This visualization illustrates the IBEX satellite in Earth orbit (the orbit reaching almost as far as the orbit of the Moon) and pulls out to beyond the heliopause boundary (the true 3-D nature of the boundary is reduced to a 2-D spherical surface). The sphere with the skymap opens to reproject the data into a near-Aitoff type map projection.The skymap shows the measured flux of energetic neutral atoms (ENAs). || ", "hits": 39 }, { "id": 10498, "url": "https://svs.gsfc.nasa.gov/10498/", "result_type": "Produced Video", "release_date": "2009-10-12T00:00:00-04:00", "title": "Keeping Up With Carbon", "description": "Carbon is all around us. This unique atom is the basic building block of life, and its compounds form solids, liquids, or gases. Carbon helps form the bodies of living organisms; it dissolves in the ocean; mixes in the atmosphere; and can be stored in the crust of the planet. A carbon atom could spend millions of years moving through this complex cycle. The ocean plays the most critical role in regulating Earth's carbon balance, and understanding how the carbon cycle is changing is key to understanding Earth's changing climate. For complete transcript, click here. || Keeping_Up_with_Carbon_640x360_ESWpage.00577_print.jpg (1024x576) [71.2 KB] || Keeping_Up_with_Carbon_640x360_ESWpage_web.png (320x180) [128.6 KB] || Keeping_Up_with_Carbon_640x360_ESWpage_thm.png (80x40) [13.9 KB] || Keeping_Up_with_Carbon_AppleTV.webmhd.webm (960x540) [84.1 MB] || Keeping_Up_with_Carbon_1280x720_ProRes.mov (1280x720) [5.1 GB] || Keeping_Up_with_Carbon_1280x720_H264.mov (1280x720) [159.3 MB] || Keeping_Up_with_Carbon_1280x720_ESWpage.mp4 (1280x720) [133.5 MB] || Keeping_Up_with_Carbon_AppleTV.m4v (960x540) [201.6 MB] || Keeping_Up_with_Carbon_640x360_ipod.m4v (640x360) [63.2 MB] || Keeping_Up_with_Carbon_640x360_ESWpage.mp4 (640x360) [63.2 MB] || Keeping_Up_with_Carbon_512x288.mpg (512x288) [123.9 MB] || Keeping_Up_with_Carbon_320x180.mp4 (320x180) [26.0 MB] || Keeping_Up_with_Carbon.wmv (320x176) [39.0 MB] || ", "hits": 160 }, { "id": 10494, "url": "https://svs.gsfc.nasa.gov/10494/", "result_type": "Produced Video", "release_date": "2009-10-09T00:00:00-04:00", "title": "The Carbon Cycle", "description": "Carbon is the basic building block of life, and these unique atoms are found everywhere on Earth. Carbon makes up Earth's plants and animals, and is also stored in the ocean, the atmosphere, and the crust of the planet. A carbon atom could spend millions of years moving through Earth in a complex cycle. This conceptual animation provides an illustration of the various parts of the Carbon cycle. Purple arrows indicate the uptake of Carbon; yellow arrows indicate the release of Carbon. On land, plants remove carbon from the atmosphere through photosynthesis. Animals eat plants and either breath out the carbon, or it moves up the food chain. When plants and animals die and decay, they transfer carbon back to the soil. Moving offshore, the ocean takes up carbon through physical and biological processes. At the ocean's surface, carbon dioxide from the atmosphere dissolves into the water. Tiny marine plants called phytoplankton use this carbon dioxide for photosynthesis. Phytoplankton are the base of the marine food web. After animals eat the plants, they breathe out the carbon or pass it up the food chain. Sometimes phytoplankton die, decompose, and are recycled in the surface waters. Phytoplankton can also sink to the bottom of the ocean, where they become buried in marine sediment. Over long time scales, this process has made the ocean floor the largest reservoir of carbon on the planet. In a process called upwelling, currents bring cold water containing carbon up to the surface. As the water warms, the carbon is then be released as a gas back into the atmosphere, continuing the carbon cycle. Carbon is found in the atmosphere as Carbon dioxide, which is a greenhouse gas. Greenhouse gases act like a blanket, and trap heat in the atmosphere. In the past two centuries, humans have increased atmospheric carbon dioxide by more than 30%, by burning fossil-fuels and cutting down forests. || ", "hits": 436 }, { "id": 10332, "url": "https://svs.gsfc.nasa.gov/10332/", "result_type": "Produced Video", "release_date": "2008-10-22T00:00:00-04:00", "title": "Solar Neutral Particles", "description": "This animation shows a charged solar particle's path leaving the sun, while following the magnetic field lines out to the heliosheath. The solar particle hits a hydrogen atom, stealing its electron and becoming neutral. We then follow it until we see it hit one of IBEX's detectors. || ", "hits": 35 }, { "id": 10133, "url": "https://svs.gsfc.nasa.gov/10133/", "result_type": "Produced Video", "release_date": "2007-07-03T00:00:00-04:00", "title": "The Helium Atom", "description": "Helium nuclei were created in the Big Bang and contain two protons and two neutrons each. Helium is the second most abundant element, comprising roughly one quarter of the mass of the Universe. This animation zooms into a standard helium atom, showing its protons (green), neutrons (white), and electrons (blue). || ", "hits": 278 }, { "id": 3056, "url": "https://svs.gsfc.nasa.gov/3056/", "result_type": "Visualization", "release_date": "2004-12-14T12:00:00-05:00", "title": "New Data from Aura's Microwave Limb Sounder (MLS) Chlorine Monoxide", "description": "The Microwave Limb Sounder (MLS) measures the chemistry of the lower stratosphere and upper troposphere. Measuring concentration of chlorine monoxide and other chemicals. Chlorine monoxide (CIO) is formed by the photolysis of CFCs in the stratosphere and the subsequent destruction of an ozone molecule, these radicals can act as a catalyst in the destruction of ozone while not being destroyed themselves. || ", "hits": 106 }, { "id": 2435, "url": "https://svs.gsfc.nasa.gov/2435/", "result_type": "Visualization", "release_date": "2002-05-09T12:00:00-04:00", "title": "IMAGE/LENA Observes Oxygen Atoms in the near-Earth Environment", "description": "Electrically charged oxygen atoms (green) are ejected into the magnetosphere due to heating in the ionosphere. The red 'thermometer' displays the intensity of the solar wind (dynamic pressure) measured by the Geotail spacecraft. The yellow 'thermometer' represents the source intensity or hydrogen counts as measured by IMAGE/LENA. || ", "hits": 27 }, { "id": 2444, "url": "https://svs.gsfc.nasa.gov/2444/", "result_type": "Visualization", "release_date": "2002-05-09T12:00:00-04:00", "title": "IMAGE/HENA Views Oxygen in the Magnetosphere (Rainbow Version)", "description": "IMAGE/HENA observes the oxygen ions, expelled from the Earth's atmosphere by the solar wind, return to the polar regions via the magnetic field. || Movie of IMAGE-HENA data using a rainbow color table for oxygen intensity. || a002444.00100_print.png (720x480) [373.3 KB] || HENArainbow_pre.jpg (320x288) [13.5 KB] || a002444.webmhd.webm (960x540) [8.1 MB] || a002444.dv (720x480) [112.3 MB] || HENArainbow.mpg (320x288) [942.9 KB] || ", "hits": 29 }, { "id": 2445, "url": "https://svs.gsfc.nasa.gov/2445/", "result_type": "Visualization", "release_date": "2002-05-09T12:00:00-04:00", "title": "IMAGE/HENA Views Oxygen in the Magnetosphere (Blue Version)", "description": "IMAGE/HENA observes the oxygen ions, expelled from the Earth's atmosphere by the solar wind, return to the polar regions via the magnetic field. || Movie of IMAGE-HENA data using a blue color table for oxygen intensity. || a002445.00010_print.png (720x480) [371.4 KB] || HENAblue_pre.jpg (320x320) [7.9 KB] || a002445.webmhd.webm (960x540) [8.1 MB] || a002445.dv (720x480) [153.6 MB] || HENAblue.mpg (320x320) [1.3 MB] || ", "hits": 26 }, { "id": 823, "url": "https://svs.gsfc.nasa.gov/823/", "result_type": "Visualization", "release_date": "1999-04-09T12:00:00-04:00", "title": "Chemical Model Animation of O2 being Broken Up and Reforming as O3", "description": "Ozone is formed when high energy ultra-violet radiation from the sun breaks apart molecular oxygen. An oxygen atom then combines with an oxygen molecule producing a new molecule with three atoms of oxygen, ozone. || ", "hits": 710 }, { "id": 824, "url": "https://svs.gsfc.nasa.gov/824/", "result_type": "Visualization", "release_date": "1999-04-09T12:00:00-04:00", "title": "Chemical Model Animation of O3 Absorbing Low-energy UV", "description": "Ozone is a strong absorber of lower energy ultraviolet radiation which can kill living organisms. This radiation is absorbed by the ozone layer when it breaks the ozone bonds. An oxygen atom is released, but the atom quickly re-combines with another oxygen molecule to regenerate ozone. || ", "hits": 411 }, { "id": 825, "url": "https://svs.gsfc.nasa.gov/825/", "result_type": "Visualization", "release_date": "1999-04-09T12:00:00-04:00", "title": "Chemical Model Animation of O3 Losing an Oxygen Atom to a Radical", "description": "Ozone is very reactive. It easily loses the third oxygen atom in the presence of other highly reactive compounds called radicals, which contain chlorine, hydrogen, nitrogen, or bromine. Minute quantities of these radicals can cause large decreases in ozone because they are not consumed in the reaction. This is called a catalytic cycle. || ", "hits": 189 } ] }