{ "count": 143, "next": "https://svs.gsfc.nasa.gov/api/search/?limit=100&offset=100&search=Solar+Rotation", "previous": null, "results": [ { "id": 14928, "url": "https://svs.gsfc.nasa.gov/14928/", "result_type": "Produced Video", "release_date": "2025-11-20T10:00:00-05:00", "title": "TESS Triples Size of Pleiades Star Cluster", "description": "These young, hot blue stars are members of the Pleiades open star cluster and reside about 430 light-years away in the northern constellation Taurus. The brightest stars are visible to the unaided eye during evenings from October to April. A new study finds the cluster to be triple the size previously thought — and shows that its stars are scattered across the night sky. The Schmidt telescope at the Palomar Observatory in California captured this color-composite image. Credit: NASA, ESA, and AURA/CaltechAlt text: Members of the Pleiades shine in blue. Image description: The Pleiades are shown in this image. Six of the stars, all blue-white, are larger than the others and have diffraction spikes and faint blue circles around them. Other, smaller blue stars are also scattered across the image. Patches of swirling blue dust surround some of the stars. || STScI-01EVVEYWX1TA3MGBK5F6EFQVGQ.jpg (4877x3513) [1.1 MB] || ", "hits": 421 }, { "id": 14883, "url": "https://svs.gsfc.nasa.gov/14883/", "result_type": "Produced Video", "release_date": "2025-08-25T11:00:00-04:00", "title": "Mapping Stellar ‘Polka Dots’", "description": "Watch to learn how a new tool uses data from exoplanets, worlds beyond our solar system, to tell us about their polka-dotted stars.Credit: NASA’s Goddard Space Flight CenterMusic: “Whimsical Whirlwinds,” Claire Leona Batchelor [PRS], Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available.Get the vertical version of this video [here](https://svs.gsfc.nasa.gov/14797/){target=_blank}. || PolkaDotStars_Thumbnail.jpg (1920x1080) [145.7 KB] || PolkaDotStars_Thumbnail_print.jpg (1024x576) [59.8 KB] || PolkaDotStars_Thumbnail_searchweb.png (320x180) [33.1 KB] || PolkaDotStars_Thumbnail_thm.png (80x40) [3.1 KB] || 14883_MappingStellarPolkaDots_Low.mp4 (1920x1080) [74.2 MB] || 14883_MappingStellarPolkaDots.mp4 (1920x1080) [262.9 MB] || MappingStellarPolkaDotsCaptions.en_US.srt [1.4 KB] || 14883_MappingStellarPolkaDots_ProRes_1920x1080_2997.mov (1920x1080) [1.4 GB] || ", "hits": 112 }, { "id": 5482, "url": "https://svs.gsfc.nasa.gov/5482/", "result_type": "Visualization", "release_date": "2025-03-17T00:00:00-04:00", "title": "An M9.4 flare from Active Region 13910 - November 25, 2024", "description": "As solar rotation carries it over the left limb of the Sun, Active Region 13910 launches an M9.4 flare.", "hits": 23 }, { "id": 5510, "url": "https://svs.gsfc.nasa.gov/5510/", "result_type": "Visualization", "release_date": "2025-02-25T17:10:00-05:00", "title": "Map of the March 29, 2025 Partial Solar Eclipse", "description": "On Saturday, March 29, 2025, the Moon passes in front of the Sun, casting its shadow across the Atlantic Ocean. Observers in Europe, western Africa, and eastern Canada are positioned to see a partial eclipse.", "hits": 410 }, { "id": 14772, "url": "https://svs.gsfc.nasa.gov/14772/", "result_type": "B-Roll", "release_date": "2025-01-29T11:00:00-05:00", "title": "Discoveries from Asteroid Bennu: Media Briefing Graphics", "description": "OSIRIS-REx MISSION RECAPThis highlight reel recaps the OSIRIS-REx mission, from assembly and launch of the spacecraft in 2016, to arrival at asteroid Bennu in 2018, TAG sample collection in 2020, the delivery of the sample to Earth in 2023, and curation of the Bennu samples in 2024.Credit: NASA || OSIRIS-REx_Collier_Present_2024_Preview_print.jpg (1024x576) [180.7 KB] || OSIRIS-REx_Collier_Present_2024_Preview.png (3840x2160) [8.3 MB] || OSIRIS-REx_Collier_Present_2024_Preview_searchweb.png (320x180) [116.3 KB] || OSIRIS-REx_Collier_Present_2024_Preview_thm.png [9.7 KB] || OSIRIS-REx_Collier_Present_2024_V3_Small.mp4 (1920x1080) [179.0 MB] || OSIRIS-REx_Collier_Present_2024_V3_Medium.mp4 (3840x2160) [500.9 MB] || OSIRIS-REx_Collier_Present_2024_V3_Large.mp4 (3840x2160) [1.6 GB] || ", "hits": 475 }, { "id": 14747, "url": "https://svs.gsfc.nasa.gov/14747/", "result_type": "Produced Video", "release_date": "2025-01-16T10:15:00-05:00", "title": "Pandora Spacecraft Animations", "description": "Animated beauty pass of an artist's concept of the Pandora spacecraft, viewed without thermal blankets, set in a neutral gray volume. Credit: NASA's Goddard Space Flight Center/Conceptual Image LabAlt text: Pandora spacecraft animation no. 1Image description: An artist’s concept of NASA’s exoplanet explorer, Pandora, floats in a light gray background. The body of the small satellite looks like a black box with metal hardware. A long metallic cylinder extends upward from the body with multiple thin rings that slightly protrude from the surface and a flat metal rectangle on one side. On the underside of the body is a shiny dark circle. Pandora’s three solar panels extend from one side of the spacecraft’s body. The visible side is gray and laced with white wires, and the panels are connected with small silver fasteners. || Pandora_Beauty_S1_Still.jpg (3840x2160) [1.0 MB] || Pandora_Beauty_S1_Still_searchweb.png (320x180) [37.2 KB] || Pandora_Beauty_S1_Still_thm.png [4.0 KB] || Pandora_Beauty_S1_1080.mp4 (1920x1080) [14.7 MB] || Pandora_Beauty_S1_4k.mp4 (3840x2160) [36.6 MB] || Pandora_Beauty_S1_ProRes_3840x2160_30.mov (3840x2160) [1.1 GB] || ", "hits": 93 }, { "id": 5423, "url": "https://svs.gsfc.nasa.gov/5423/", "result_type": "Visualization", "release_date": "2024-11-27T11:00:00-05:00", "title": "Gravity waves disturbing the stratospheric polar vortex", "description": "Animation 1: Changes in temperature and height on the surface of 850 Kelvin potential temperature. The mountain generated gravity waves create strong cooling  as the gravity waves propagate through the stratosphere, while the polar vortex (the cold blue ring) evolves to become colder. || stratospher850_039_T.02498_print.jpg (1024x576) [108.0 KB] || stratospher850_039_T.02498_searchweb.png (320x180) [50.4 KB] || stratospher850_039_T.02498_thm.png (80x40) [4.2 KB] || stratospher850_039_T_1080p30.mp4 (1920x1080) [52.0 MB] || stratospher850_039_T [0 Item(s)] || stratospher850_039_T.mp4 (3840x2160) [148.7 MB] || stratospher850_039_T.mp4.hwshow || ", "hits": 104 }, { "id": 5344, "url": "https://svs.gsfc.nasa.gov/5344/", "result_type": "Visualization", "release_date": "2024-10-15T14:00:00-04:00", "title": "Solar Cycle 25 - the Solar Magnetic Field from Solar Minimum to Pole Flip", "description": "One advantage of long-lived missions like Solar Dynamics Observatory (SDO) is the ability to see slow but significant changes over long periods of time.This view from SDO's Helioseismic and Magnetic Imager (HMI) shows the evolution of sunspots on the solar disk starting from solar minimum (around December 2019) and into the maximum solar activity phase. The video ends in September 2024, however this maximum phase is expected to continue into 2025.", "hits": 475 }, { "id": 5378, "url": "https://svs.gsfc.nasa.gov/5378/", "result_type": "Visualization", "release_date": "2024-09-07T15:30:00-04:00", "title": "Map of the October 2, 2024 Annular Solar Eclipse", "description": "On Wednesday, October 2, 2024, the Moon passes in front of the Sun, casting its shadow across the Pacific Ocean. Observers on Rapa Nui (Easter Island) and in far southern Chile and Argentina are in the path of the annular eclipse. Hawai'i, parts of Antarctica, and the southern half of South America see a partial eclipse.", "hits": 222 }, { "id": 5326, "url": "https://svs.gsfc.nasa.gov/5326/", "result_type": "Visualization", "release_date": "2024-07-18T12:00:00-04:00", "title": "Moon Essentials: Orbit", "description": "The mean (average) orbit of the Moon as it changes over the course of 8.5 years. Shows the tilt of the orbit and the slow rotation of the nodes (where the Moon's orbit intersects the orbit plane of the Earth) and the apses (the near and far points). This is a simplified model that ignores the short-term influence of the Sun and the rest of the solar system. || simple.1351_print.jpg (1024x576) [62.0 KB] || simple.1351_searchweb.png (320x180) [39.1 KB] || simple.1351_thm.png (80x40) [3.0 KB] || simple [0 Item(s)] || moon_orbit_simple_1080p30.mp4 (1920x1080) [9.1 MB] || moon_orbit_simple_720p30.mp4 (1280x720) [5.0 MB] || moon_orbit_simple_360p30.mp4 (640x360) [2.3 MB] || ", "hits": 5134 }, { "id": 5199, "url": "https://svs.gsfc.nasa.gov/5199/", "result_type": "Visualization", "release_date": "2024-06-24T16:10:00-04:00", "title": "Moon Essentials: Libration in Latitude", "description": "A 2-frame GIF showing the extremes of lunar libration in latitude. || liblat.gif (1080x1080) [1.1 MB] ||", "hits": 455 }, { "id": 5195, "url": "https://svs.gsfc.nasa.gov/5195/", "result_type": "Visualization", "release_date": "2024-06-24T16:00:00-04:00", "title": "Moon Essentials: Libration in Longitude", "description": "A 2-frame GIF showing the extremes of lunar libration in longitude. || liblon.gif (1080x1080) [1.1 MB] || ", "hits": 759 }, { "id": 14573, "url": "https://svs.gsfc.nasa.gov/14573/", "result_type": "Produced Video", "release_date": "2024-04-25T10:00:00-04:00", "title": "Nancy Grace Roman Space Telescope Reaction Wheel and Thruster Animations", "description": "Beauty pass of Roman, coming over the top of the solar panels.Credit: NASA's Goddard Space Flight Center/CI Lab || RST_Beauty_S1_4K_60_ProRes.00458_print.jpg (1024x576) [164.9 KB] || RST_Beauty_S1_1080.mp4 [19.0 MB] || RST_Beauty_S1_4K_60.mp4 [92.2 MB] || RST_Beauty_S1_4K_60_ProRes.webm [10.4 MB] || RST_Beauty_S1_4K_60_ProRes.mov [2.0 GB] || ", "hits": 77 }, { "id": 14525, "url": "https://svs.gsfc.nasa.gov/14525/", "result_type": "Produced Video", "release_date": "2024-04-23T12:00:00-04:00", "title": "Moving Roman - Reaction Wheels", "description": "Moving Roman: Reaction Wheels. Watch this video to learn more about how reaction wheels work and how they will be an essential part of pointing the Nancy Grace Roman Space Telescope.Credit: NASA's Goddard Space Flight Center.Music credit: \"Breaking the Code\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Moving_Roman_Reaction_Wheels_Still.jpg (1920x1080) [613.0 KB] || Moving_Roman_Reaction_Wheels_Still_searchweb.png (320x180) [67.7 KB] || Moving_Roman_Reaction_Wheels_Still_thm.png (80x40) [6.0 KB] || 14525_MovingRoman_ReactionWheels_Good.webm (1920x1080) [23.2 MB] || 14525_MovingRoman_ReactionWheels_Good.mp4 (1920x1080) [153.7 MB] || 14525_MovingRoman_ReactionWheels_Best.mp4 (1920x1080) [531.5 MB] || 14525_MovingRoman_ReactionWheels_Captions.en_US.srt [4.7 KB] || 14525_MovingRoman_ReactionWheels_Captions.en_US.vtt [4.4 KB] || 14525_MovingRoman_ReactionWheels_ProRes_1920x1080_2997.mov (1920x1080) [2.7 GB] || ", "hits": 222 }, { "id": 5220, "url": "https://svs.gsfc.nasa.gov/5220/", "result_type": "Visualization", "release_date": "2024-03-12T00:00:00-04:00", "title": "X3.3 flare at Active Region 13575 - February 9, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Just days after an eruption, Active Region 13575, now carried by solar rotation just over the lower right limb of the solar disk, launches an X3.3 class flare. For details of this event, see the Space Weather database entry. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "hits": 15 }, { "id": 5225, "url": "https://svs.gsfc.nasa.gov/5225/", "result_type": "Visualization", "release_date": "2024-03-12T00:00:00-04:00", "title": "X2.5 flare at Active Region 13576 - February 16, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13576, now carried by solar rotation to the lower right limb of the solar disk, launches an X2.5 class flare. For details of this event, see the Space Weather database entry. Lots of post-flare filament activity on the limb, particularly solar material falling back towards the Sun.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "hits": 20 }, { "id": 5222, "url": "https://svs.gsfc.nasa.gov/5222/", "result_type": "Visualization", "release_date": "2024-02-20T12:07:00-05:00", "title": "5000 Years of Total Solar Eclipses", "description": "A heatmap showing the frequency of total solar eclipses over the 5000 years from 2000 BCE to 3000 CE. Includes versions without the color key and without the continent outlines. || eclipse_freq_heatmap_print.jpg (1024x512) [323.0 KB] || eclipse_freq_heatmap_searchweb.png (320x180) [120.8 KB] || eclipse_freq_heatmap_thm.png (80x40) [17.8 KB] || eclipse_freq_heatmap.tif (5400x2700) [14.9 MB] || eclipse_freq_heatmap_nocbar.tif (5400x2700) [14.9 MB] || eclipse_freq_heatmap_noland.tif (5400x2700) [17.0 MB] || ", "hits": 528 }, { "id": 5216, "url": "https://svs.gsfc.nasa.gov/5216/", "result_type": "Visualization", "release_date": "2024-02-15T00:00:00-05:00", "title": "M6.8 flare at Active Region 13559 - January 29, 2024", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.Active Region 13559 now carried by solar rotation to the upper right limb of the solar disk, launches a mid-range (M6.8 class) flare. For details of this event, see the Space Weather database entry. A large arcade of plasma loops forms after the event, more visible in the 171 angstrom and 304 angstrom filters. An eclipse of the Sun by Earth provides a nice 'curtain close' for the event. For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "hits": 38 }, { "id": 5206, "url": "https://svs.gsfc.nasa.gov/5206/", "result_type": "Visualization", "release_date": "2024-02-13T00:00:00-05:00", "title": "X5.0 flare (\"New Years Eve Flare\") at Active Region 13536 - December 31, 2023", "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.The Sun, getting more active as it continues towards the peak of Solar Cycle 25, ends 2023 with a bang as Active Region 13536 on the left limb erupts with an X 5.0 flare, the largest observed so far this cycle. Note that this is probably the same active region (just renumbered) which launched an X2.8 flare a couple weeks earlier (X2.8 flare at Active Region 13514 - December 14, 2023), when solar rotation carried this region over the right limb of the Sun. For details of this event, see the Space Weather database entry.For more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to all this imagery. || ", "hits": 21 }, { "id": 40505, "url": "https://svs.gsfc.nasa.gov/gallery/hyperwall-power-playlist-planetary-science-focus/", "result_type": "Gallery", "release_date": "2023-08-28T00:00:00-04:00", "title": "Hyperwall Power Playlist - Planetary Science Focus", "description": "This is a collection of our most powerful, newsworthy, and frequently used Hyperwall-ready visualizations, along with several that haven't gotten the attention they deserve. They're especially great for more general or top-level science talks, or to \"set the scene\" before a deep dive into a more focused subject or dataset. We've tried to cover the subject areas our speakers focus on most. \n\nIf you're not seeing what you're looking for, there is a huge library of visualizations more localized or specialized in subject - please use the Search function above, and filter \"Result type\" for \"Hyperwall Visual.\"\n\n If you'd like to use one of these visualizations in your Hyperwall presentation, we'll need to know which element on which page. On the visualization's web page, below the visual you'd like to use, you'll see a Link icon next to the Download button. All we need is for you to click on that icon and include that link in your presentation Powerpoint/Keynote or visualization list. Additionally, please check our Hyperwall How-To Guide for tips on designing your Hyperwall presentation, file specifications, and Powerpoint/Keynote templates.", "hits": 285 }, { "id": 40518, "url": "https://svs.gsfc.nasa.gov/gallery/hyperwall-power-playlist-astrophysics-focus/", "result_type": "Gallery", "release_date": "2023-08-28T00:00:00-04:00", "title": "Hyperwall Power Playlist - Astrophysics Focus", "description": "This is a collection of our most powerful, newsworthy, and frequently used Hyperwall-ready visualizations, along with several that haven't gotten the attention they deserve. They're especially great for more general or top-level science talks, or to \"set the scene\" before a deep dive into a more focused subject or dataset. We've tried to cover the subject areas our speakers focus on most. \n\nIf you're not seeing what you're looking for, there is a huge library of visualizations more localized or specialized in subject - please use the Search function above, and filter \"Result type\" for \"Hyperwall Visual.\"\n\n If you'd like to use one of these visualizations in your Hyperwall presentation, we'll need to know which element on which page. On the visualization's web page, below the visual you'd like to use, you'll see a Link icon next to the Download button. All we need is for you to click on that icon and include that link in your presentation Powerpoint/Keynote or visualization list. Additionally, please check our Hyperwall How-To Guide for tips on designing your Hyperwall presentation, file specifications, and Powerpoint/Keynote templates.", "hits": 320 }, { "id": 14209, "url": "https://svs.gsfc.nasa.gov/14209/", "result_type": "Produced Video", "release_date": "2023-01-09T17:10:00-05:00", "title": "NASA’s Compton Mission Glimpses Supersized Neutron Stars", "description": "This simulation tracks the gravitational wave and density changes as two orbiting neutron stars crash together. Dark purple colors represent the lowest densities, while yellow-white shows the highest. An audible tone and a visual frequency scale (at left) track the steady rise in the frequency of gravitational waves as the neutron stars close. When the objects merge at 42 seconds, the gravitational waves suddenly jump to frequencies of thousands of hertz and bounce between two primary tones (quasiperiodic oscillations, or QPOs). The presence of these signals in such simulations led to the search and discovery of similar phenomena in the light emitted by short gamma-ray bursts.Credit: NASA's Goddard Space Flight Center and STAG Research Centre/Peter HammondComplete transcript available.Watch this video on the NASA Goddard YouTube channel.Visual description:On a black background with a faint gray grid, two multicolored blobs representing merging neutron stars circle and close. The colors indicate density. Yellow-white indicates the highest densities, at the centers of the objects. The colors change to orange and red at their periphery, with purple colors representing matter torn from and swirling with the neutron stars as they orbit. The grid shrinks as the camera pulls back to capture a wider view of the merger. A pale orange display at left shows the changing frequency of the gravitational waves generated, which is also indicated by the rising tone. As the merger occurs, the screen shows a spinning yellow blob at center immersed in a large cloud of magneta and purple debris. || Merger_Simulation_Annotated_Still_2.jpg (1920x1080) [180.7 KB] || 14209_Hypermassive_QPO_Simulation_Zoom_YOUTUBE_1080.webm (1920x1080) [12.1 MB] || 14209_Hypermassive_QPO_Simulation_Zoom_YOUTUBE_1080.mp4 (1920x1080) [129.3 MB] || 14209_Hypermassive_QPO_Simulation_Zoom_YOUTUBE_BEST_1080.mp4 (1920x1080) [161.8 MB] || 14209_NS_Merger_QPO_SRT_Captions.en_US.srt [1.6 KB] || 14209_NS_Merger_QPO_SRT_Captions.en_US.vtt [1.6 KB] || 14209_Hypermassive_QPO_Simulation_Zoom_YOUTUBE_ProRes_1920x1080_2997.mov (1920x1080) [1.0 GB] || ", "hits": 254 }, { "id": 40447, "url": "https://svs.gsfc.nasa.gov/gallery/visualizationsfor-educators/", "result_type": "Gallery", "release_date": "2022-08-17T00:00:00-04:00", "title": "Visualizations for Educators", "description": "Phenomena are observable events that occur in nature. Data visualizations can offer new ways for students to experience and explore Earth and space phenomena that happen over large scales of time and at great distances. This gallery includes visualizations of phenomena that support topics that are taught in middle and high school and are aligned with select Next Generation Science Standards.\n\n\nThis gallery was curated by Anne Arundle County Science Teachers Margaret Graham and Jeremy Milligan with support from Dr. Rachel Connolly during the summer of 2022. A video showing how Jeremy Milligan uses SVS resources to develop a phenomena-based lesson is also available.", "hits": 300 }, { "id": 14115, "url": "https://svs.gsfc.nasa.gov/14115/", "result_type": "Produced Video", "release_date": "2022-03-08T13:00:00-05:00", "title": "NASA's NICER Tracks a Magnetar's Hot Spots", "description": "Explore how NASA’s Neutron star Interior Composition Explorer (NICER) tracked brilliant hot spots on the surface of an erupting magnetar – from 13,000 light-years away. Credit: NASA's Goddard Space Flight CenterMusic: \"Particles and Fields\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Magnetar_Still.jpg (1920x1080) [574.3 KB] || Magnetar_Still_print.jpg (1024x576) [229.0 KB] || Magnetar_Still_searchweb.png (320x180) [66.1 KB] || Magnetar_Still_thm.png (80x40) [5.2 KB] || 14115_Merging_Magnetar_HotSpots_1080_Best.webm (1920x1080) [17.4 MB] || 14115_Merging_Magnetar_HotSpots_1080.mp4 (1920x1080) [158.9 MB] || 14115_Merging_Magnetar_HotSpots_1080_Best.mp4 (1920x1080) [382.0 MB] || 14115_Migrating_Magnetar_HotSpots_1080.en_US.srt [2.1 KB] || 14115_Migrating_Magnetar_HotSpots_1080.en_US.vtt [2.1 KB] || 14115_Merging_Magnetar_HotSpots_ProRes_1920x1080_2997.mov (1920x1080) [2.1 GB] || ", "hits": 224 }, { "id": 13933, "url": "https://svs.gsfc.nasa.gov/13933/", "result_type": "Produced Video", "release_date": "2021-09-28T13:00:00-04:00", "title": "Lucy L-20 Briefing", "description": "NASA will hold a virtual media briefing at 2 p.m. EDT Tuesday, Sept. 28, to preview the launch of the agency’s first spacecraft to study Jupiter’s Trojan asteroids. The Trojan asteroids are remnants of the early solar system clustered in two “swarms” leading and following Jupiter in its path around the Sun.The live briefing will stream on NASA Television, the agency's website, NASA’s Twitter account and the NASA App.Participants in Tuesday's briefing will include:• Alana Johnson, Senior Communications Specialist, NASA Planetary Science Division• Lori Glaze, director of NASA's Planetary Science Division at NASA Headquarters in Washington.• Hal Levison, Lucy Principal Investigator, Southwest Research Institute in Boulder, Colorado.• Keith Noll, Lucy Project Scientist, NASA’s Goddard Space Flight Center in Greenbelt, Maryland. • Rich Lipe, Lockheed Marin Spacecraft Program Manager, Denver, Colorado. • Donya Douglas-Bradshaw, Lucy Project Manager, NASA Goddard Space Flight Center in Greenbelt, Maryland.Over its 12-year primary mission, Lucy will explore a record number of asteroids in separate orbits around the Sun. The spacecraft will fly by one asteroid in the solar system’s main belt, located between the orbits of Mars and Jupiter, followed by seven Trojans. In addition, Lucy’s path will circle back to Earth three times for gravity assists, making it the first spacecraft ever to travel out to the distance of Jupiter and return to the vicinity of Earth.The Lucy mission is named after the fossilized skeleton of an early hominin (pre-human ancestor) discovered in Ethiopia in 1974 and named “Lucy” by the team of paleoanthropologists who discovered it. Just as the Lucy fossil provided unique insights into humanity’s evolution, the Lucy mission promises to revolutionize our knowledge of planetary origins and the formation of the solar system.Lucy is scheduled to launch no earlier than Saturday, Oct. 16, on a United Launch Alliance Atlas V 401 rocket from Space Launch Complex-41 at Cape Canaveral Space Force Station, Florida.Southwest Research Institute is the home institution of the principal investigator. NASA Goddard Space provides overall mission management, systems engineering, plus safety and mission assurance. Lockheed Martin Space built the spacecraft. Lucy is the 13th mission in NASA’s Discovery Program. NASA’s Marshall Space Flight Center in Huntsville, Alabama, manages the Discovery Program for the Science Mission Directorate. The launch is managed by NASA’s Launch Services Program based at Kennedy Space Center in Florida.For more information about Lucy, visit: http://www.nasa.gov/lucy || ", "hits": 29 }, { "id": 10662, "url": "https://svs.gsfc.nasa.gov/10662/", "result_type": "Produced Video", "release_date": "2021-04-14T00:00:00-04:00", "title": "Webb Science Simulations: Planetary Systems and Origins of Life", "description": "Supercomputer simulations of planeratry evolution. Part 1: Turbulent Molecular Cloud Nebula with Protostellar ObjectsThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk and Michael Norman to visualize a computational data set of a turbulent molecular cloud nebula forming protostellar objects and accretion disks approximately 100 AU in diameter, on the order of the size of our solar system. AVL used its Amore software to interpolate and render the Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics. The AMR simulation was developed by Drs. Kritsuk and Norman at the Laboratory for Computational Astrophysics. The AMR simulation generated more than 2 terabytes of data and follows star formation processes in a self-gravitating turbulent molecular cloud with a dynamic range of half-a-million in linear scale, resolving both the large-scale filamentary structure of the molecular cloud (~5 parsec) and accretion disks around emerging young protostellar objects (down to 2 AU). Part 2: Protoplanetary Disk and Planet FormationThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Dr. Aaron Boley to visualize the 16,000 year evolution of a young, isolated protoplanetary disk which surrounds a newly-formed protostar. The disk forms spiral arms and a dense clump as a result of gravitational collapse. Dr. Aaron Boley developed this computational model to investigate the response of young disks to mass accretion from their surrounding envelopes, including the direct formation of planets and brown dwarfs through gravitational instability. The main formation mechanism for gas giant planets has been debated within the scientific community for over a decade. One of these theories is 'direct formation through gravitational instability.' If the self-gravity of the gas overwhelms the disk's thermal pressure and the stabilizing effect of differential rotation, the gas closest to the protostar rotates faster than gas farther away. In this scenario, regions of the gaseous disk collapse and form a planet directly. The study, presented in Boley (2009), explores whether mass accretion in the outer regions of disks can lead to such disk fragmentation. The simulations show that clumps can form in situ at large disk radii. If the clumps survive, they can become gas giants on wide orbits, e.g., Fomalhaut b, or even more massive objects called brown dwarfs. Whether a disk forms planets at large radii and, if so, the number of planets that form, depend on how much of the envelope mass is distributed at large distances from the protostar. The results of the simulations suggest that there are two modes of gas giant planet formation. The first mode occurs early in the disk's lifetime, at large radii, and through the disk instability mechanism. After the main accretion phase is over, gas giants can form in the inner disk, over a period of a million years, through the core accretion mechanism, which researchers are addressing in other studies.Thanks to R. H. Durisen, L. Mayer, and G. Lake for comments and discussions relating to this research. This study was supported in part by the University of Zurich, Institute for Theoretical Physics, and by a Swiss Federal Grant. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.AVL at NCSA, University of Illinois. || ", "hits": 219 }, { "id": 13794, "url": "https://svs.gsfc.nasa.gov/13794/", "result_type": "Infographic", "release_date": "2021-02-12T14:00:00-05:00", "title": "NASA’s TESS Finds New Worlds in a River of Stars", "description": "This illustration sketches out the main features of TOI 451, a triple-planet system located 400 light-years away in the constellation Eridanus.Credit: NASA’s Goddard Space Flight Center || TOI_451_infographic_1920.png (1920x1080) [2.6 MB] || TOI_451_infographic_1920_print.jpg (1024x576) [129.4 KB] || TOI_451_infographic_3840.png (3840x2160) [8.2 MB] || TOI_451_infographic_1920_searchweb.png (320x180) [73.0 KB] || TOI_451_infographic_1920_thm.png (80x40) [6.5 KB] || ", "hits": 355 }, { "id": 13778, "url": "https://svs.gsfc.nasa.gov/13778/", "result_type": "Produced Video", "release_date": "2020-12-03T17:00:00-05:00", "title": "Solar Activity Continues to Rise with 'Anemone' Eruption", "description": "Short video showing the solar flare and subsequent prominence eruption and \"arcade\" of loops.Credit: NASA/GSFC/SDOMusic: \"Beautiful Awesome\" from Universal Production MusicWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Anemone_Eruption_131-171_Blend.jpg (1920x1080) [281.9 KB] || Anemone_Eruption_131-171_Blend_searchweb.png (180x320) [78.6 KB] || Anemone_Eruption_131-171_Blend_thm.png (80x40) [6.6 KB] || 13778_Anemone_Eruption_ProRes_1920x1080_2997.mov (1920x1080) [2.0 GB] || 13778_Anemone_Eruption_Best_1080.mp4 (1920x1080) [718.2 MB] || 13778_Anemone_Eruption_1080.mp4 (1920x1080) [220.6 MB] || 13778_Anemone_Eruption_Best_1080.webm (1920x1080) [16.0 MB] || AnemoneEruption_SRT_Captions.en_US.srt [500 bytes] || AnemoneEruption_SRT_Captions.en_US.vtt [513 bytes] || ", "hits": 56 }, { "id": 13664, "url": "https://svs.gsfc.nasa.gov/13664/", "result_type": "Produced Video", "release_date": "2020-07-16T08:00:00-04:00", "title": "ESA and NASA Release First Images From Solar Orbiter Mission", "description": "Scientists from ESA (European Space Agency) and NASA will present the first images captured by Solar Orbiter, the joint ESA/NASA mission to study the Sun, during an online news briefing at 8 a.m. EDT Thursday, July 16. Launched on Feb. 9, 2020, Solar Orbiter turned on all 10 of its instruments together for the first time in mid-June as it made its first close pass of the Sun. The flyby captured the closest images ever taken of the Sun. During the briefing, mission experts will discuss what these closeup images reveal about our star, including what we can learn from Solar Orbiter’s new measurements of particles and magnetic fields flowing from the Sun.The briefing will stream live at:https://www.nasa.gov/solarorbiterfirstlight/Participants in the call include:•Daniel Müller – Solar Orbiter Project Scientist at ESA•Holly R. Gilbert – Solar Orbiter Project Scientist at NASA•José Luis Pellón Bailón – Solar Orbiter Deputy Spacecraft Operations Manager at ESA•David Berghmans – Principal investigator of the Extreme Ultraviolet Imager (EUI) at the Royal Observatory of Belgium•Sami Solanki – Principal investigator of the Polarimetric and Helioseismic Imager (PHI) and director of the Max Planck Institute for Solar System Research•Christopher J. Owen – Principal investigator of the Solar Wind Analyser (SWA) at Mullard Space Science Laboratory, University College London•ESA’s first light images•ESA press release •NASA feature story || ", "hits": 204 }, { "id": 40413, "url": "https://svs.gsfc.nasa.gov/gallery/earth-science-playlist/", "result_type": "Gallery", "release_date": "2020-04-01T00:00:00-04:00", "title": "Earth Science Playlist", "description": "No description available.", "hits": 1 }, { "id": 40409, "url": "https://svs.gsfc.nasa.gov/gallery/fermi-stills/", "result_type": "Gallery", "release_date": "2020-01-22T00:00:00-05:00", "title": "Fermi Stills", "description": "A collection of Fermi-related still images, illustrations, graphics and short clips.", "hits": 301 }, { "id": 4755, "url": "https://svs.gsfc.nasa.gov/4755/", "result_type": "Visualization", "release_date": "2019-12-12T14:00:00-05:00", "title": "Mars Upper Level Winds Observed by MAVEN - Visualizations", "description": "MAVEN observes upper level Martian winds over the course of about two years. || maven_upper_winds_60fps.0104__cam_mainShape_190909182423_beauty.1780_print.jpg (1024x576) [42.9 KB] || maven_upper_winds_60fps.0104__cam_mainShape_190909182423_beauty.1780_searchweb.png (320x180) [49.1 KB] || maven_upper_winds_60fps.0104__cam_mainShape_190909182423_beauty.1780_thm.png (80x40) [4.0 KB] || maven_upper_winds_campaigns_1080p60.mp4 (1920x1080) [51.0 MB] || maven_upper_winds_campaigns_1080p30.mp4 (1920x1080) [46.4 MB] || maven_upper_winds.0104_cam_mainShape_190909182423_beauty_1080p30.webm (1920x1080) [9.6 MB] || campaigns (3840x2160) [0 Item(s)] || maven_upper_winds_campaigns_2160p60.mp4 (3840x2160) [162.2 MB] || maven_upper_winds_campaigns_2160p30.mp4 (3840x2160) [146.8 MB] || 4755_MAVEN_Wind_Currents_Full.mov (3840x2160) [9.7 GB] || maven_upper_winds_campaigns_1080p30.mp4.hwshow [201 bytes] || ", "hits": 60 }, { "id": 13266, "url": "https://svs.gsfc.nasa.gov/13266/", "result_type": "Produced Video", "release_date": "2019-07-31T10:00:00-04:00", "title": "TESS Discovery Leads to Surprising Find of Promising World", "description": "Tour the GJ 357 system, located 31 light-years away in the constellation Hydra. Astronomers confirming a planet candidate identified by NASA’s Transiting Exoplanet Survey Satellite subsequently found two additional worlds orbiting the star. The outermost planet, GJ 357 d, is especially intriguing to scientists because it receives as much energy from its star as Mars does from the Sun. Credit: NASA's Goddard Space Flight CenterWatch this video on the NASA Goddard YouTube channel.Music: \"Golden Temple\" from Killer Tracks.Complete transcript available.See the bottom of the page for a version without on-screen text. || tess_gj357_english_thm.jpg (1920x1080) [798.7 KB] || tess_gj357_english_thm_print.jpg (1024x576) [291.4 KB] || tess_gj357_english_thm_searchweb.png (180x320) [79.3 KB] || tess_gj357_english_thm_web.png (320x180) [79.3 KB] || tess_gj357_english_thm_thm.png (80x40) [5.7 KB] || tess_gj357_english_HQ.webm (1920x1080) [15.6 MB] || tess_gj357_english_LQ.mp4 (1920x1080) [139.2 MB] || tess_gj357_english_HQ.mp4 (1920x1080) [259.3 MB] || tess_gj357_english.en_US.srt [2.4 KB] || tess_gj357_english.en_US.vtt [2.4 KB] || tess_gj357_english_prores.mov (1920x1080) [1.4 GB] || ", "hits": 310 }, { "id": 13223, "url": "https://svs.gsfc.nasa.gov/13223/", "result_type": "Produced Video", "release_date": "2019-06-27T09:00:00-04:00", "title": "TESS Discovers Its Tiniest World To Date", "description": "NASA’s Transiting Exoplanet Survey Satellite has confirmed the tiniest planet in its catalog so far — one of three discovered around a bright, nearby star called L 98-59. As shown in the illustrations in this video, all could occupy the “Venus zone,” the range of distances from the star where a Venus-like atmosphere is possible. The outermost planet also has the potential for a Neptune-like atmosphere. Credit: NASA’s Goddard Space Flight CenterMusic: \"Autumn Rush\" from Killer TracksComplete transcript available.Watch this video on the NASA Goddard YouTube channel. || tess_smallest_planet_preview.jpg (1920x1080) [288.5 KB] || tess_smallest_planet_preview_print.jpg (1024x576) [118.1 KB] || tess_smallest_planet_preview_searchweb.png (320x180) [53.2 KB] || tess_smallest_planet_preview_web.png (320x180) [53.2 KB] || tess_smallest_planet_preview_thm.png (80x40) [5.5 KB] || tess_smallest_planet_HQ.mp4 (1920x1080) [245.9 MB] || tess_smallest_planet_LQ.mp4 (1920x1080) [190.0 MB] || tess_smallest_planet_prores.mov (1920x1080) [1.3 GB] || tess_smallest_planet_HQ.webm (1920x1080) [14.8 MB] || tess_smallest_planet.en_US.srt [1.9 KB] || tess_smallest_planet.en_US.vtt [1.9 KB] || ", "hits": 167 }, { "id": 31036, "url": "https://svs.gsfc.nasa.gov/31036/", "result_type": "Hyperwall Visual", "release_date": "2019-04-30T00:00:00-04:00", "title": "Jupiter or Earth?", "description": "Side by side images show similar features despite being from different planets. || jupiter_earth_with_scalebar_print.jpg (1024x576) [100.2 KB] || jupiter_earth_with_scalebar.png (3840x2160) [5.6 MB] || jupiter_earth_with_scalebar_searchweb.png (320x180) [93.5 KB] || jupiter_earth_with_scalebar_thm.png (80x40) [6.7 KB] || jupiter_earth_with_scalebar.hwshow [216 bytes] || ", "hits": 224 }, { "id": 40357, "url": "https://svs.gsfc.nasa.gov/gallery/sdo4k-content/", "result_type": "Gallery", "release_date": "2018-09-13T09:22:28-04:00", "title": "SDO: 4k Content", "description": "Since 2010, the Solar Dynamics Observatory has taken 60 million images of the sun and 2 comets. Here are a few of our favorites.", "hits": 311 }, { "id": 40355, "url": "https://svs.gsfc.nasa.gov/gallery/sdo/", "result_type": "Gallery", "release_date": "2018-08-31T00:00:00-04:00", "title": "SDO – Solar Dynamics Observatory", "description": "Since its launch on Feb. 11, 2010, the Solar Dynamics Observatory (SDO) has studied the solar atmosphere to help us understand the Sun’s influence on Earth. Every 12 seconds, SDO images the Sun in 10 wavelengths of ultraviolet light, each of which reveals different solar features. These images help us explain where the Sun's energy comes from, how the inside of the Sun works, and how the Sun’s atmosphere stores and releases energy in dramatic eruptions that can influence Earth.\n\nLearn more: https://science.nasa.gov/mission/sdo/", "hits": 855 }, { "id": 13030, "url": "https://svs.gsfc.nasa.gov/13030/", "result_type": "Produced Video", "release_date": "2018-08-06T10:00:00-04:00", "title": "NASA's Planet-Hunting TESS Catches a Comet Before Starting Science", "description": "This video is compiled from a series of images taken on July 25 by the Transiting Exoplanet Survey Satellite. The angular extent of the widest field of view is six degrees. Visible in the images are the comet C/2018 N1, asteroids, variable stars, asteroids and reflected light from Mars. TESS is expected to find thousands of planets around other nearby stars. Credit: Massachusetts Institute of Technology/NASA’s Goddard Space Flight CenterWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || TESS_Comet_Still.jpg (1920x1080) [409.0 KB] || TESS_Comet_Still_print.jpg (1024x576) [112.2 KB] || TESS_Comet_Still_searchweb.png (320x180) [50.8 KB] || TESS_Comet_Still_thm.png (80x40) [3.8 KB] || 13030_TESS_Comet_ProRes_1080_2997.mov (1920x1080) [1.7 GB] || 13030_TESS_Comet_1080.mp4 (1920x1080) [118.6 MB] || 13030_TESS_Comet_H264_1080_Best.mov (1920x1080) [173.0 MB] || 13030_TESS_Comet_H264_1080_Good.m4v (1920x1080) [114.8 MB] || 13030_TESS_Comet_ProRes_1080_2997.webm (1920x1080) [10.8 MB] || 13030_TESS_Comet_SRT_Captions.en_US.srt [1.3 KB] || 13030_TESS_Comet_SRT_Captions.en_US.vtt [1.3 KB] || ", "hits": 50 }, { "id": 4663, "url": "https://svs.gsfc.nasa.gov/4663/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Earth's Magnetosphere", "description": "A simple visualization of Earth's magnetosphere near the time of the equinox. || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_print.jpg (1024x576) [139.2 KB] || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_searchweb.png (320x180) [91.9 KB] || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_thm.png (80x40) [6.1 KB] || Equinox_Dayside-noglyph (1920x1080) [0 Item(s)] || Earth_Equinox_Dayside.HD1080i_p30.webm (1920x1080) [13.0 MB] || Earth_Equinox_Dayside.HD1080i_p30.mp4 (1920x1080) [240.4 MB] || Equinox_Dayside-noglyph (3840x2160) [0 Item(s)] || Earth_Equinox_Dayside_2160p30.mp4 (3840x2160) [642.0 MB] || Earth_Equinox_Dayside.HD1080i_p30.mp4.hwshow [199 bytes] || ", "hits": 190 }, { "id": 4664, "url": "https://svs.gsfc.nasa.gov/4664/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Jupiter's Magnetosphere", "description": "Jupiter's magnetosphere - a basic view. || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_print.jpg (1024x576) [245.3 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_searchweb.png (320x180) [132.5 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_thm.png (80x40) [8.3 KB] || JupiterBasic-noglyph (1920x1080) [0 Item(s)] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.webm (1920x1080) [32.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [406.6 MB] || JupiterBasic-noglyph (3840x2160) [0 Item(s)] || Jupiter_JupiterBasic_Dayside_2160p30.mp4 (3840x2160) [984.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ", "hits": 172 }, { "id": 4665, "url": "https://svs.gsfc.nasa.gov/4665/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Saturn's Magnetosphere", "description": "A basic view of Saturn's magnetosphere. || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [186.2 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.8 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [7.1 KB] || SaturnBasic-noglyph (1920x1080) [0 Item(s)] || Saturn_SaturnBasic_Dayside.HD1080i_p30.webm (1920x1080) [22.1 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [365.5 MB] || SaturnBasic-noglyph (3840x2160) [0 Item(s)] || Saturn_SaturnBasic_Dayside_2160p30.mp4 (3840x2160) [938.9 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4.hwshow || ", "hits": 115 }, { "id": 4666, "url": "https://svs.gsfc.nasa.gov/4666/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Uranus' Magnetosphere", "description": "A basic view of the Uranian magnetosphere when the rotation axis is perpendicular to the Uranus-Sun line and days and nights are of equal duration. || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [197.1 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.3 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || UranusEquinox-noglyph (1920x1080) [0 Item(s)] || Uranus_UranusEquinox_Dayside.HD1080i_p30.webm (1920x1080) [20.9 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4 (1920x1080) [308.1 MB] || UranusEquinox-noglyph (3840x2160) [0 Item(s)] || Uranus_UranusEquinox_Dayside_2160p30.mp4 (3840x2160) [758.5 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ", "hits": 108 }, { "id": 4667, "url": "https://svs.gsfc.nasa.gov/4667/", "result_type": "Visualization", "release_date": "2018-07-27T00:00:00-04:00", "title": "Neptune's Magnetosphere", "description": "A basic view of the Neptunian magnetosphere when the southern side of the rotation axis is directed sunward (southern summer) || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [195.5 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [108.2 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || NeptuneSouthSummer-noglyph (1920x1080) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.webm (1920x1080) [21.4 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4 (1920x1080) [328.8 MB] || NeptuneSouthSummer-noglyph (3840x2160) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside_2160p30.mp4 (3840x2160) [820.2 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4.hwshow [212 bytes] || ", "hits": 178 }, { "id": 12999, "url": "https://svs.gsfc.nasa.gov/12999/", "result_type": "Produced Video", "release_date": "2018-07-12T15:00:00-04:00", "title": "Parker Solar Probe Path Across Sun's Surface", "description": "The velocity of Parker Solar Probe is fastest right at perihelion. The spacecraft is so fast that near perihelion, it flies faster than the Sun rotates. This animation illustrates this by following the track of the spacecraft on map of the surface of the Sun. When the spacecraft flies faster than the Sun rotates, the orbit track on the surface goes backward (retrograde). At the turning points (labeled co-rotation periods), the spacecraft and the Sun are essential moving together (co-rotation). These periods of time, which last many hours, will be invaluable for making continuous measurements of solar wind from the same source.Credit: NASA/JPL/WISPR Team || 12999_PSPRelativeMotionToSun2018V81080p.00001_print.jpg (1024x576) [100.7 KB] || 12999_PSPRelativeMotionToSun2018V81080p.00001_searchweb.png (320x180) [54.3 KB] || 12999_PSPRelativeMotionToSun2018V81080p.00001_web.png (320x180) [54.3 KB] || 12999_PSPRelativeMotionToSun2018V81080p.00001_thm.png (80x40) [3.5 KB] || 12999_PSPRelativeMotionToSun2018V81080p.mp4 (1920x1080) [76.2 MB] || PRORES_B-ROLL_12999_PSPRelativeMotionToSun2018V81080p_prores.mov (1280x720) [335.3 MB] || YOUTUBE_1080_12999_PSPRelativeMotionToSun2018V81080p_youtube_1080.mp4 (1920x1080) [71.6 MB] || NASA_TV_12999_PSPRelativeMotionToSun2018V81080p.mpeg (1280x720) [156.1 MB] || 12999_PSPRelativeMotionToSun2018V81080p.webm (1920x1080) [3.7 MB] || 12999_PSPRelativeMotionToSun2018V81080p_appletv.m4v (1280x720) [22.9 MB] || NASA_PODCAST_12999_PSPRelativeMotionToSun2018V81080p_ipod_sm.mp4 (320x240) [6.6 MB] || ", "hits": 154 }, { "id": 30969, "url": "https://svs.gsfc.nasa.gov/30969/", "result_type": "Hyperwall Visual", "release_date": "2018-06-18T10:00:00-04:00", "title": "M101 (Pinwheel Galaxy)", "description": "This animation shows the Messier 101 (Pinwheel) Galaxy, with simulated rotation, in visible, then infrared, then X-ray, and finally all three combined. || STScI-H-M101_1x-1920x1080.00001_print.jpg (1024x576) [150.4 KB] || STScI-H-M101_1x-1920x1080.00001_searchweb.png (320x180) [99.4 KB] || STScI-H-M101_1x-1920x1080.00001_thm.png (80x40) [6.3 KB] || STScI-H-M101_1x-1280x720.mp4 (1280x720) [18.1 MB] || STScI-H-M101_1x-1920x1080.mp4 (1920x1080) [50.6 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-M101_1x-1920x1080.webm (1920x1080) [5.6 MB] || STScI-H-M101_1x-640x360.mp4 (640x360) [7.8 MB] || STScI-H-M101_1x-3840x2160.mp4 (3840x2160) [32.3 MB] || STScI-H-M101_1x-H265-3840x2160.mp4 (3840x2160) [11.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 215 }, { "id": 4623, "url": "https://svs.gsfc.nasa.gov/4623/", "result_type": "Visualization", "release_date": "2018-04-30T10:00:00-04:00", "title": "The Dynamic Solar Magnetic Field with Introduction", "description": "This narrated visualization transitions from a view of the Sun in visible light, to a view in ultraviolet light showing the plasma flowing along solar magnetic structures, to the underlying magnetic field of the solar photosphere, to a model construction of magnetic fieldlines above the photosphere.This video is also available on our YouTube channel. || SolarMagnetism_UHD3840.04000_print.jpg (1024x576) [198.9 KB] || SolarMagnetism_UHD3840.04000_thm.png (80x40) [6.0 KB] || SolarMagnetism_UHD3840.04000_web.png (320x180) [84.1 KB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.webm (1280x720) [33.9 MB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.mov (1280x720) [7.4 GB] || SolarMagnetism_ProRes3_UHD2160_p30_Narrated.mov (3840x2160) [12.8 GB] || ", "hits": 119 }, { "id": 12808, "url": "https://svs.gsfc.nasa.gov/12808/", "result_type": "Produced Video", "release_date": "2018-01-10T14:10:00-05:00", "title": "Newly Renamed Swift Mission Catches a Comet Slowdown", "description": "NASA’s Swift satellite detected an unprecedented slowdown in the rotation of comet 41P/Tuttle-Giacobini-Kresák when it passed nearest to Earth in early 2017. Watch to learn more.Credit: NASA’s Goddard Space Flight Center Music: \"Valley of Crystals\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Comet_3.jpg (1920x1080) [159.1 KB] || Comet_3_print.jpg (1024x576) [49.1 KB] || Comet_3_searchweb.png (320x180) [41.5 KB] || Comet_3_thm.png (80x40) [4.3 KB] || 12808_Swift_Comet_Spin_ProRes_1920x1080_2997.mov (1920x1080) [2.4 GB] || 12808_Swift_Comet_Spin-H264_Best_1080p.mov (1920x1080) [503.7 MB] || 12808_Swift_Comet_Spin_H264_Good_1080.m4v (1920x1080) [196.4 MB] || 12808_Swift_Comet_Spin-H264_Best_1080p.webm (1920x1080) [22.2 MB] || 12808_Swift_Comet_Spin_SRT_Caption.en_US.srt [3.4 KB] || 12808_Swift_Comet_Spin_SRT_Caption.en_US.vtt [3.2 KB] || ", "hits": 61 }, { "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": 1024 }, { "id": 40338, "url": "https://svs.gsfc.nasa.gov/gallery/parker-solar-probe/", "result_type": "Gallery", "release_date": "2017-09-22T00:00:00-04:00", "title": "Parker Solar Probe", "description": "On a mission to “touch the Sun,” NASA's Parker Solar Probe became the first spacecraft to fly through the corona — the Sun’s upper atmosphere — passing within 3.8 million miles of the solar surface during its closest approaches. Parker Solar Probe flies through the corona at speeds up to 430,000 mph taking measurements to help scientists better understand the fundamental drivers of solar activity and space weather events that can impact life on Earth. Facing brutal heat and radiation conditions, Parker Solar Probe employs four instrument suites designed to study electric and magnetic fields, plasma, waves and energetic particles, as well as image the solar wind, the constant stream of material released by the Sun. \n\nParker Solar Probe launched on Aug. 12, 2018, from the Cape Canaveral Air Force Station.\n\nLearn more: https://science.nasa.gov/mission/parker-solar-probe/", "hits": 694 }, { "id": 40337, "url": "https://svs.gsfc.nasa.gov/gallery/lrosolar-eclipse/", "result_type": "Gallery", "release_date": "2017-07-17T00:00:00-04:00", "title": "LRO and Solar Eclipse Events", "description": "This page features videos for the 2017 Solar Eclipse Events being coordinated with the LRO Mission production team.", "hits": 127 }, { "id": 4143, "url": "https://svs.gsfc.nasa.gov/4143/", "result_type": "Visualization", "release_date": "2017-07-12T10:01:00-04:00", "title": "Saturn's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 105 }, { "id": 4141, "url": "https://svs.gsfc.nasa.gov/4141/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Earth's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. For this Earth visualization, note that the north magnetic pole points out of the southern hemisphere.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann and Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 228 }, { "id": 4142, "url": "https://svs.gsfc.nasa.gov/4142/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Jupiter's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The volcanic activity on Jupiter's moon Io launches a large amount of sulfur-based compounds along its orbit, which is subsequently ionized by solar ultraviolet radiation. This is represented in the visualization by the yellowish structure along the orbit of Io. This creates a plasma torus and ring current around Jupiter, which alters the planet's magnetic field, forming some of the perturbations in Jupiter's magnetic field along the orbit of Io.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann and Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 270 }, { "id": 4144, "url": "https://svs.gsfc.nasa.gov/4144/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Uranus' Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Uranus is tilted over ninety degrees relative to the revolution axis of the solar system, placing it roughly in the plane of the solar system. In addition, the magnetic axis has a large tilt relative to the rotation axis. These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Uranus' magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 308 }, { "id": 4145, "url": "https://svs.gsfc.nasa.gov/4145/", "result_type": "Visualization", "release_date": "2017-07-12T10:00:00-04:00", "title": "Neptune's Magnetosphere", "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes). The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Neptune is highly tilted relative to the revolution axis of the solar system, but nowhere near as extreme as Uranus. It's magnetic axis also has a large tilt relative to the rotation axis. These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines. Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun. The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis. The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis. It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center. ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Neptune's magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ", "hits": 259 }, { "id": 4579, "url": "https://svs.gsfc.nasa.gov/4579/", "result_type": "Visualization", "release_date": "2017-06-21T05:00:00-04:00", "title": "Flying Around The Eclipse Shadow", "description": "A view of the Moon's shadow during the August 21, 2017 eclipse from both the night and day sides of the Earth. || night_to_day.0300_print.jpg (1024x576) [47.6 KB] || night_to_day.0300_searchweb.png (320x180) [28.2 KB] || night_to_day.0300_thm.png (80x40) [3.2 KB] || eclipse_flyaround_1080p30.mp4 (1920x1080) [36.2 MB] || eclipse_flyaround_720p30.mp4 (1280x720) [12.7 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || eclipse_flyaround_720p30.webm (1280x720) [5.4 MB] || eclipse_flyaround_720p30.wmv (1280x720) [42.8 MB] || FlyingAroundTheEclipseShadow.mov (1280x720) [682.8 MB] || eclipse_flyaround_360p30.mp4 (640x360) [4.3 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || eclipse_flyaround_2160p30.mp4 (3840x2160) [122.4 MB] || FlyingAroundTheEclipseShadow4k.mov (3840x2160) [2.4 GB] || eclipse_flyaround_1080p30.mp4.hwshow [222 bytes] || ", "hits": 92 }, { "id": 12613, "url": "https://svs.gsfc.nasa.gov/12613/", "result_type": "Produced Video", "release_date": "2017-06-02T11:00:00-04:00", "title": "SDO 4k Slow-rotation Sun Resource Page", "description": "Still Image for page || SDO_Slow_Gallery.jpg (1920x1080) [235.4 KB] || SDO_Slow_Gallery_searchweb.png (320x180) [43.0 KB] || SDO_Slow_Gallery_thm.png (80x40) [3.6 KB] || ", "hits": 164 }, { "id": 4559, "url": "https://svs.gsfc.nasa.gov/4559/", "result_type": "Visualization", "release_date": "2017-04-27T10:00:00-04:00", "title": "Kepler Stares at Neptune", "description": "In late 2014 and early 2015, NASA's Kepler telescope observed the eighth planet in our solar system, Neptune. Kepler detected Neptune's daily rotation, the movement of clouds, and even minute changes in the sun's brightness, paving the way for future studies of weather and climate beyond our solar system. Complete transcript available.Watch this video on the NASA Goddard YouTube channel.Music Provided by Killer Tracks:\"Lost Contact\" – Adam Salkeld & Neil Pollard\"Processing Thoughts\" – Theo Golding || Neptune-Triton-Zoom-Thumbnail.jpg (1920x1080) [1.2 MB] || 4559_Kepler_Neptune_Twitter_720.mp4 (1280x720) [30.6 MB] || WEBM-4559_Kepler_Neptune_APR.webm (960x540) [58.6 MB] || Neptune-Triton-Zoom-Thumbnail_Big.tiff (1920x1080) [11.9 MB] || 4559_Kepler_Neptune_Facebook_720.mp4 (1280x720) [173.0 MB] || 4559_Kepler_Neptune_Captions_Output.en_US.srt [2.8 KB] || 4559_Kepler_Neptune_Captions_Output.en_US.vtt [2.9 KB] || 4559_Kepler_Neptune_APR.mov (1920x1080) [1.9 GB] || 4559_Kepler_Neptune_APR_4444.mov (1920x1080) [4.1 GB] || 4559_Kepler_Neptune_APR.mov.hwshow [205 bytes] || ", "hits": 105 }, { "id": 20267, "url": "https://svs.gsfc.nasa.gov/20267/", "result_type": "Animation", "release_date": "2017-04-26T00:00:00-04:00", "title": "Neutron Star Animations", "description": "The Neutron star Interior Composition Explorer (NICER) mission will study neutron stars, the densest known objects in the cosmos. These neutron star animations and graphics highlight some of their unique characteristics.For more information about NICER visit: nasa.gov/nicer. || ", "hits": 475 }, { "id": 4557, "url": "https://svs.gsfc.nasa.gov/4557/", "result_type": "Visualization", "release_date": "2017-03-15T10:00:00-04:00", "title": "Leaky Radiation Belts", "description": "This visualization opens with a full view of the radiation belt of trapped electrons circling Earth. We open a slice of the belts, to display a cross-section for clarity and move the camera to a more equatorial view. Earth rotation and solar motion have been turned off for this visualization to reduce distracting additional motions. || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_print.jpg (1024x576) [113.8 KB] || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_searchweb.png (180x320) [83.0 KB] || LeakyBelts_FullData_ObliqueIntro.slate_CRTT.HD1080i.0600_thm.png (80x40) [6.0 KB] || ObliqueIntro (1920x1080) [0 Item(s)] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.mp4 (1920x1080) [77.0 MB] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.webm (1920x1080) [5.5 MB] || ObliqueIntro (3840x2160) [0 Item(s)] || LeakyBelts_FullData_ObliqueIntro.UHD2160_p30.mp4 (3840x2160) [279.0 MB] || LeakyBelts_FullData_ObliqueIntro.HD1080i_p30.mp4.hwshow [210 bytes] || ", "hits": 110 }, { "id": 12399, "url": "https://svs.gsfc.nasa.gov/12399/", "result_type": "Produced Video", "release_date": "2016-10-27T12:55:00-04:00", "title": "NASA's Kepler, Swift Missions Harvest ‘Pumpkin’ Stars", "description": "Dive into the Kepler field and learn more about the origins of these rapidly spinning stars.Credit: NASA's Goddard Space Flight CenterMusic: \"Electric Cosmos\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Pumpkin_Star_Still.png (1920x1080) [10.8 MB] || Pumpkin_Star_Still_print.jpg (1024x576) [85.7 KB] || Pumpkin_Star_Still_searchweb.png (320x180) [66.5 KB] || Pumpkin_Star_Still_thm.png (80x40) [4.4 KB] || 12399_Swift_Pumpkin_Star2_ProRes_1920x1080_2997.mov (1920x1080) [2.0 GB] || 12399_Swift_Pumpkin_Star_FINAL2_youtube_hq.mov (1920x1080) [1.2 GB] || 12399_Swift_Pumpkin_Star2_H264_1080.mov (1920x1080) [221.8 MB] || 12399_Swift_Pumpkin_Star2_1080_Good.m4v (1920x1080) [147.1 MB] || 12399_Swift_Pumpkin_Star2_1080_Most_Compatible.m4v (960x540) [59.7 MB] || 12399_Swift_Pumpkin_Star_FINAL2_HD.wmv (1920x1080) [332.6 MB] || 12399_Swift_Pumpkin_Star2_ProRes_1920x1080_2997.webm (1920x1080) [17.0 MB] || 12399_Swift_Pumpkin_Star_SRT_Captions.en_US.srt [2.3 KB] || 12399_Swift_Pumpkin_Star_SRT_Captions.en_US.vtt [2.3 KB] || 12399_Swift_Pumpkin_Star_FINAL2_ipod_sm.mp4 (320x240) [26.8 MB] || ", "hits": 88 }, { "id": 12379, "url": "https://svs.gsfc.nasa.gov/12379/", "result_type": "Produced Video", "release_date": "2016-09-28T10:00:00-04:00", "title": "Space Radiation Highlights", "description": "A collection of space radiation highlights featuring:NASA's Van Allen ProbesNASA's CubeSats || ", "hits": 153 }, { "id": 12151, "url": "https://svs.gsfc.nasa.gov/12151/", "result_type": "Produced Video", "release_date": "2016-02-12T13:00:00-05:00", "title": "NASA On Air: NASA's SDO Satellite Captures HD Time Lapse Of The Sun (2/12/2016)", "description": "LEAD: NASA's Solar Dynamics Observatory catches the sun in HD video. 1: Images shown here are in the extreme ultraviolet range. 2: The temperature of the solar material is near 1 million degrees F.3: It's easy to see the sun's rotation, 1 full rotation every 25 days. TAG: Scientists study these images to better understand the solar flares and solar explosions called coronal mass ejections that can sometimes disrupt our technology such as GPS systems. || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_1920x1080_print.jpg (1024x576) [97.7 KB] || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_1920x1080_searchweb.png (320x180) [52.5 KB] || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_1920x1080_thm.png (80x40) [4.2 KB] || WSI_WEATHER_CHANNEL_NASAonAir-SDOYr6-_1920x1080.mov (1920x1080) [681.2 MB] || WSI_WEATHER_CHANNEL_NASAonAir-SDOYr6-_1280x720.mov (1280x720) [737.5 MB] || NBC_TODAY_NASAonAir-SDOYr6-_NBC_Today.mov (1920x1080) [75.4 MB] || WeatherChannel_NASAonAir-SDOYr6-WeatherChannel.wmv (1280x720) [7.4 MB] || Accuweather_NASAonAir-SDOYr6-Accuweather.avi (1280x720) [5.8 MB] || BARON_SERVICE_NASAonAir-SDOYr6-_baron.mp4 (1920x1080) [25.9 MB] || WC_PRORES_422_NASAonAir-SDOYr6-_prores.mov (1920x1080) [508.1 MB] || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_960x540.m4v (960x540) [31.3 MB] || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_1280x720.m4v (1280x720) [58.8 MB] || IPAD_DELIVERABLES_NASAonAir-SDOYr6-_iPad_1920x1080.m4v (1920x1080) [94.0 MB] || WEBM_NASAonAir-SDOYr6-.webm (960x540) [14.3 MB] || ", "hits": 183 }, { "id": 12144, "url": "https://svs.gsfc.nasa.gov/12144/", "result_type": "Produced Video", "release_date": "2016-02-12T09:00:00-05:00", "title": "SDO: Year 6", "description": "This ultra-high definition (3840x2160) video shows the sun in the 171 angstrom wavelength of extreme ultraviolet light. It covers a time period of January 2, 2015 to January 28, 2016 at a cadence of one frame every hour, or 24 frames per day. This timelapse is repeated with narration by solar scientist Nicholeen Viall and contains close-ups and annotations. 171 angstrom light highlights material around 600,000 Kelvin and shows features in the upper transition region and quiet corona of the sun. The video is available to download here at 59.94 frames per second, double the rate YouTube currently allows for UHD content. The music is titled \"Tides\" and is from Killer Tracks.Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year6_HCblend_HD.png (1920x1080) [5.3 MB] || SDO_Year6_HCblend_HD.jpg (1920x1080) [545.9 KB] || SDO_Year6_HCblend_HD_print.jpg (1024x576) [179.5 KB] || SDO_Year6_HCblend_UHD.png (3840x2160) [19.7 MB] || SDO_Year6_HCblend_UHD.jpg (3840x2160) [1.2 MB] || SDO_Year6_HCblend_HD_searchweb.png (180x320) [59.6 KB] || SDO_Year6_HCblend_HD_thm.png (80x40) [4.8 KB] || 12144_SDO_Year_6_appletv.webm (1280x720) [50.5 MB] || 12144_SDO_Year_6_appletv.m4v (1280x720) [241.9 MB] || 12144_SDO_Year_6_appletv_appletv_subtitles.m4v (1280x720) [242.1 MB] || SDO_Year_6_SRT_Captions.en_US.srt [6.3 KB] || SDO_Year_6_SRT_Captions.en_US.vtt [6.3 KB] || 12144_SDO_Year_6_H264_Good_1920x1080_2997.mov (1920x1080) [1.4 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_2997.mov (3840x2160) [9.1 GB] || 12144_SDO_Year_6_H264_Good_3840x2160_5994.mov (3840x2160) [10.2 GB] || 12144_SDO_Year_6_ProRes_3840x2160_5994.mov (3840x2160) [50.3 GB] || ", "hits": 108 }, { "id": 4319, "url": "https://svs.gsfc.nasa.gov/4319/", "result_type": "Visualization", "release_date": "2016-02-11T00:00:00-05:00", "title": "Solar Dynamics Observatory: April 21, 2015 Eruption on the Solar Limb", "description": "Movie of plasma eruption (upper left limb). || Apr2015LimbErupt_304A_stand.HD1080i.00945_print.jpg (1024x576) [73.9 KB] || Apr2015LimbErupt_304A_stand.HD1080i.00945_searchweb.png (320x180) [41.0 KB] || Apr2015LimbErupt_304A_stand.HD1080i.00945_thm.png (80x40) [3.5 KB] || Apr2015LimbErupt_304A_stand_1080p.webm (1920x1080) [6.4 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Apr2015LimbErupt_304A_stand_1080p.mp4 (1920x1080) [43.2 MB] || Apr2015LimbErupt_304A_stand_1080p.mp4.hwshow [199 bytes] || ", "hits": 37 }, { "id": 4391, "url": "https://svs.gsfc.nasa.gov/4391/", "result_type": "Visualization", "release_date": "2016-01-29T10:00:00-05:00", "title": "The Dynamic Solar Magnetic Field", "description": "A visualization of the slow changes of the solar magnetic field over the course of four years. || PFSSbasicView_inertial.HD1080i.0400_print.jpg (1024x576) [168.7 KB] || PFSSbasicView_inertial.HD1080i.0400_searchweb.png (180x320) [78.9 KB] || PFSSbasicView_inertial.HD1080i.0400_thm.png (80x40) [5.8 KB] || PFSSbasicView_inertial_1080p30.webm (1920x1080) [18.1 MB] || PFSSbasicView (1920x1080) [128.0 KB] || PFSSbasicView_inertial_1080p30.mp4 (1920x1080) [326.6 MB] || PFSSbasicView_inertial_1080p10.mp4 (1920x1080) [470.2 MB] || PFSSbasicView_HD1080p10.mov (1920x1080) [804.4 MB] || PFSSbasicView_inertial_1080p30.mp4.hwshow [232 bytes] || ", "hits": 129 }, { "id": 12101, "url": "https://svs.gsfc.nasa.gov/12101/", "result_type": "Produced Video", "release_date": "2016-01-04T00:00:00-05:00", "title": "Fermi Hyperwall--2016 AAS Technical", "description": "Upresed 5760x3240 animation of the Fermi spacecraft.Credit: NASA's Goddard Space Flight Center/CI Lab || frame-000020_print.jpg (1024x576) [147.2 KB] || Fermi_Beauty_EarthandStars_1080p.webm (1920x1080) [1.4 MB] || Fermi_Beauty_EarthandStars_1080p.mov (1920x1080) [25.4 MB] || FermiBeautyDraft (5760x3240) [0 Item(s)] || Fermi_Beauty_EarthandStars_4k.mov (4096x2304) [47.9 MB] || Fermi_Beauty_EarthandStars_4k_ProRes.mov (5760x3240) [808.7 MB] || ", "hits": 92 }, { "id": 40271, "url": "https://svs.gsfc.nasa.gov/gallery/live-shots-gallery/", "result_type": "Gallery", "release_date": "2015-11-27T00:00:00-05:00", "title": "Live Shots Gallery Collection", "description": "Collection of live shot pages of b-roll and interviews!", "hits": 521 }, { "id": 12021, "url": "https://svs.gsfc.nasa.gov/12021/", "result_type": "Produced Video", "release_date": "2015-10-13T13:00:00-04:00", "title": "Hubble Maps Jupiter in 4k Ultra HD", "description": "New imagery from the Hubble Space Telescope is revealing details never before seen on Jupiter. Hubble’s new Jupiter maps were used to create this Ultra HD animation.Watch this video on the NASA Explorer YouTube channel. || JupiterThumbnailSmall.png (2160x1215) [1.4 MB] || G2015-085_Jupiter720_MASTER_appletv_appletv_subtitles.m4v (1280x720) [39.0 MB] || G2015-085_Jupiter720_MASTER_appletv.m4v (1280x720) [39.0 MB] || WEBM_G2015-085_Jupiter4k_MASTER_YouTube.webm (960x540) [28.5 MB] || G2015-085_Jupiter720_MASTER.mp4 (1280x720) [98.9 MB] || G2015-085_Jupiter720_MASTER_nasa_tv.mpeg (1280x720) [249.3 MB] || G2015-085_Jupiter720_MASTER_prores.mov (1280x720) [917.9 MB] || G2015-085_Jupiter720_MASTER.en_US.srt [98 bytes] || G2015-085_Jupiter720_MASTER.en_US.vtt [111 bytes] || G2015-085_Jupiter720_.key [41.8 MB] || G2015-085_Jupiter720_.pptx [39.3 MB] || G2015-085_Jupiter720_MASTER_12021.key [41.7 MB] || G2015-085_Jupiter720_MASTER_12021.pptx [39.3 MB] || G2015-085_Jupiter4k_MASTER_YouTube.mp4 (3840x2160) [495.9 MB] || G2015-085_Jupiter4k_MASTER.mov (3840x2160) [4.5 GB] || G2015-085_Jupiter4k_MASTER_YouTube.hwshow [94 bytes] || G2015-085_Jupiter720_MASTER_appletv.m4v.hwshow [88 bytes] || ", "hits": 1022 }, { "id": 40111, "url": "https://svs.gsfc.nasa.gov/gallery/astro-star/", "result_type": "Gallery", "release_date": "2015-09-18T00:00:00-04:00", "title": "Astrophysics Star Listing", "description": "No description available.", "hits": 177 }, { "id": 40247, "url": "https://svs.gsfc.nasa.gov/gallery/goes/", "result_type": "Gallery", "release_date": "2015-09-14T00:00:00-04:00", "title": "GOES", "description": "GOES (Geostationary Operational Environmental Satellites) is a joint mission between NOAA and NASA. GOES-1 was launched in October of 1975 providing weather forecasters with a one-of-a-kind view of Earth. Since then, each generation of GOES satellites improved allowing for a near real-time view of the Western Hemisphere. \n\n GOES satellites orbit 22,236 miles above Earth’s equator, at speeds equal to the Earth's rotation. This allows them to maintain their positions over specific geographic regions so they can provide continuous coverage of that area over time.\n\nThe GOES-R series of satellites, designated with a letter during development and renamed with a number after reaching geostationary orbit, have transformed NOAA’s geostationary weather monitoring capabilities. \n\nGOES-R (now GOES-16) launched in 2016 and operates as NOAA’s GOES East satellite. GOES-S (now GOES-17), launched in 2018 and serves as an on-orbit backup. GOES-T (now GOES-18) launched in 2022 and is NOAA’s operational GOES West satellite. The final satellite in the series, GOES-U (GOES-19), was launched on June 25, 2024, and is slated to replace GOES-16 in the GOES East position by spring 2025.\n\nTogether, GOES East and GOES West watch over more than half the globe — from the west coast of Africa to New Zealand and from near the Arctic Circle to the Antarctic Circle. \n\nThe GOES-R Program is a collaborative effort between NOAA and NASA. NASA builds and launches the satellites for NOAA, which operates them and distributes their data to users worldwide.", "hits": 272 }, { "id": 40227, "url": "https://svs.gsfc.nasa.gov/gallery/suneclipse2017/", "result_type": "Gallery", "release_date": "2015-06-11T00:00:00-04:00", "title": "Solar Eclipse 2017", "description": "During the solar eclipse on August 21, 2017, the Moon's shadow will pass over all of North America. The path of the umbra, where the eclipse is total, stretches from Salem, Oregon to Charleston, South Carolina. This will be the first total solar eclipse visible in the contiguous United States in 38 years.\nDuring those brief moments when the moon completely blocks the sun’s bright face for 2 + minutes, day will turn into night, making visible the otherwise hidden solar corona, the sun’s outer atmosphere. Bright stars and planets will become visible as well. This is truly one of nature’s most awesome sights.\rThe eclipse provides a unique opportunity to study the sun, Earth, moon and their interaction because of the eclipse’s long path over land coast to coast. Scientists will be able to take ground-based and airborne observations over a period of an hour and a half to complement the wealth of data provided by NASA assets.\nVisit https://eclipse2017.nasa.gov for more information.", "hits": 247 }, { "id": 11817, "url": "https://svs.gsfc.nasa.gov/11817/", "result_type": "Produced Video", "release_date": "2015-03-20T10:00:00-04:00", "title": "TESS Mission Trailer", "description": "This video is a trailer of the upcoming TESS mission. || Screen_Shot_2015-03-19_at_6.13.34_PM.png (1271x715) [803.1 KB] || Screen_Shot_2015-03-19_at_6.13.34_PM_searchweb.png (180x320) [69.7 KB] || Screen_Shot_2015-03-19_at_6.13.34_PM_web.png (320x180) [69.7 KB] || Screen_Shot_2015-03-19_at_6.13.34_PM_thm.png (80x40) [11.1 KB] || TESS_Final_youtube_hq.mov (1280x720) [52.6 MB] || TESS_Final.mov (1280x720) [1.3 GB] || TESS_Final_1280x720.wmv (1280x720) [47.4 MB] || TESS_Final_appletv.m4v (960x540) [44.6 MB] || TESS_Final_appletv.webm (960x540) [13.1 MB] || TESS_Final_appletv_subtitles.m4v (960x540) [44.6 MB] || TESS_Final_nasaportal.mov (640x360) [39.1 MB] || TESS_Final_ipod_lg.m4v (640x360) [18.9 MB] || TESS.en_US.srt [1.3 KB] || TESS_Final_ipod_sm.mp4 (320x240) [9.7 MB] || ", "hits": 136 }, { "id": 4279, "url": "https://svs.gsfc.nasa.gov/4279/", "result_type": "Visualization", "release_date": "2015-03-11T12:00:00-04:00", "title": "Magnetospheric Reconnection - July 2012", "description": "Profile view of magnetosphere. Density data slice in x-z plane. || Earth_Reconnect-July2012mII_Profile.noslate_GSEmove.HD1080i.0818_print.jpg (1024x576) [135.8 KB] || Earth_Reconnect-July2012mII_Profile.HD1080.mov (1920x1080) [377.5 MB] || Profile (1920x1080) [256.0 KB] || Earth_Reconnect-July2012mII_Profile_HD1080.mp4 (1920x1080) [141.3 MB] || Earth_Reconnect-July2012mII_Profile.HD1080.webm (1920x1080) [11.3 MB] || ", "hits": 1707 }, { "id": 4225, "url": "https://svs.gsfc.nasa.gov/4225/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "title": "The M7 Flare of October 2, 2014, seen from SDO", "description": "In this 171 ångstrom image, the group of coronal loops on the lower right of the solar limb launches a stream of plasma. || Oct2014Mflare_171A_stand.HD1080i.00748_print.jpg (1024x576) [68.2 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_searchweb.png (320x180) [46.9 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_thm.png (80x40) [4.4 KB] || Oct2014Mflare_171A_stand.HD1080i.00748_web.png (320x180) [46.9 KB] || Oct2014Mflare_171A_stand_1080.mp4 (1920x1080) [23.2 MB] || Oct2014Mflare_171A (1920x1080) [128.0 KB] || Oct2014Mflare_171A_stand_720.mp4 (1280x720) [9.7 MB] || Oct2014Mflare_171A_stand_720.webmhd.webm (960x540) [2.9 MB] || Oct2014Mflare_171A_stand_360.mp4 (640x360) [2.6 MB] || ", "hits": 24 }, { "id": 4232, "url": "https://svs.gsfc.nasa.gov/4232/", "result_type": "Visualization", "release_date": "2015-02-11T00:00:00-05:00", "title": "Twelve Days of AR12192 from SDO and GOES", "description": "SDO 131 angstrom visual with overlaid plot of GOES X-ray flux during the time span. || AR12192_131_GOES.composite.01500_print.jpg (1024x1024) [274.5 KB] || AR12192_131_GOES.composite.01500_searchweb.png (320x180) [72.8 KB] || AR12192_131_GOES.composite.01500_thm.png (80x40) [6.4 KB] || AR12192_131_GOES.composite.01500_web.png (320x320) [102.2 KB] || AR12192_131_GOES-composite_1024.webm (1024x1024) [13.7 MB] || AR12192_131_GOES-composite_1024.mp4 (1024x1024) [312.6 MB] || Composite (4096x4096) [0 Item(s)] || AR12192_131_GOES-composite_1024_4232.pptx [62.0 MB] || AR12192_131_GOES-composite_1024_4232.key [64.5 MB] || AR12192_131_GOES.mp4 (4096x4096) [5.3 GB] || ", "hits": 35 }, { "id": 11691, "url": "https://svs.gsfc.nasa.gov/11691/", "result_type": "Produced Video", "release_date": "2014-12-23T11:00:00-05:00", "title": "Tornadoes On The Sun?", "description": "NASA’s Solar Dynamics Observatory (SDO) stares at our sun in high-definition from space. Under the spacecraft's constant gaze the sun's invisible magnetic field betrays its presence by bending charged gas, or plasma, into entrancing patterns. In February 2012, SDO captured curious images in which plasma near the sun’s surface appears to swirl like debris in a tornado. But was the plasma really rotating? Some scientists believe the spinning is an illusion caused by a 2-D projection of 3-D motion, while others think it is truly twisting. Newer observations may show more clearly that some of the material is moving toward Earth while some is moving away, pointing to genuine rotation. If that’s the case, bunched magnetic fields at the sun’s surface could be causing the elaborate plasma dance by becoming tangled themselves. Watch the video to see solar magnetism in action. || ", "hits": 217 }, { "id": 4217, "url": "https://svs.gsfc.nasa.gov/4217/", "result_type": "Visualization", "release_date": "2014-10-08T00:00:00-04:00", "title": "Coordinated Earth: Measuring Space in the Near-Earth Environment", "description": "When we operate satellites in space, they are often taking measurements along the locations of their travel. As with many measurements, they are only useful if they can be placed in the proper context - their relationship to other measurements at the same, and different, locations. To assemble these measurements within context, we also need to know where and when the measurements were taken, and to do that, we need to define a coordinate system.In three-dimensional space, we define a position with three numbers, relative to a point we define as the Origin of the coordinate system, defined as (0,0,0). Each number represents a distance from the origin along one of three directions. We usually defined these directions by axes, labelled X, Y, and Z, which are defined to be mutually perpendicular, each one is at right angles to the others.While all coordinate systems are equal, all coordinate systems are not equally convenient for a given problem of interest. Sometimes the data and mathematics we use for exploring different problems can be more complex in one coordinate system or another. To simplify this, we often define a number of different coordinate systems and ways to do transformations between them.In studying the space environment around Earth, we find five different coordinate systems of use. Geocentric (GEO): This is the coordinate system useful for measuring things close to Earth’s surface. The origin is chosen at the center of Earth. The x-axis points from the center of Earth through the Prime Meridian (by convention chosen as the meridian in Greenwich, London, UK (longitude = 0). The z-axis points towards the north geographic pole. Geocentric Earth Inertial (GEI): This coordinate system is fixed relative to the distant stars, so Earth rotates about the z-axis relative to it. The origin of this coordinate system is at the center of the Earth. The x-axis points to the first point in Aries (Wikipedia: Vernal Equinox) and the z-axis points to the north geographic & celestial pole. The direction of the celestial pole changes due to Earth’s rotational precession (Wikipedia). Geocentric Solar Ecliptic (GSE): The origin is at the center of the Earth. The x-axis is along the line between Earth and the Sun. The z-axis is the north ecliptic pole and is fixed in direction (but for slow changes due to Earth orbital changes). Solar Magnetic (SM): the origin is at the center of the Earth. The z-axis is chosen parallel to the Earth magnetic dipole axis. The y-axis is chosen to be perpendicular to the z-axis and the Earth-Sun line (pointing towards dusk). Geocentric Solar Magnetospheric (GSM): The origin is at the center of the Earth. The x-axis is defined as the Earth-Sun line (same as in GSE). The y-axis is defined to be perpendicular to the plane containing the x-axis and the magnetic dipole axis so the magnetic axis always lies in this plane.Similar coordinate systems are defined for the Sun and other planets of the Solar System.Development Note: This visualization was originally developed to test coordinate system transformations in the visualization framework.References:C. T. Russell. \"Geophysical coordinate transformations\". Cosmical Electrodynamics 2, 184-196 (1971). URL.M.A. Hapgood. \"Space Physics Coordinate Transformations: A User Guide\". Planetary & Space Science, 40, 711-717.(1992). URLSPENVIS Help Pages: Coordinate Systems and transformations || ", "hits": 166 }, { "id": 4158, "url": "https://svs.gsfc.nasa.gov/4158/", "result_type": "Visualization", "release_date": "2014-04-10T00:00:00-04:00", "title": "Lunar Eclipses and the Moon's Orbit", "description": "The animations on this page illustrate the Moon’s orbit and its role in lunar and solar eclipses. A solar eclipse happens when the Moon’s shadow falls on the Earth, while a lunar eclipse happens when the Earth’s shadow falls on the Moon.Eclipses can only happen at New and Full Moon, when the Earth, Moon, and Sun are all in a straight line. But they don’t happen every New and Full Moon, because the Moon’s orbit is tilted by about 5 degrees. As the Earth and Moon travel around the Sun, the tilt of the Moon’s orbit changes direction relative to the Sun.This is analogous to the way the tilt of the Earth causes seasons. Just like winter and summer happen every six months, eclipses tend to occur on a roughly six-month cycle.Unlike most eclipse shadow diagrams, the first three animations here don’t greatly exaggerate the scale of the Earth and Moon. They are only 2x their true scale. The view is exactly perpendicular to the Earth-Sun line. The angle of the Moon’s orbital tilt and the “tapering” of the shadows are both accurate. The orbit happens to be calculated for the months preceding the April 15, 2014 total lunar eclipse. || ", "hits": 634 }, { "id": 11497, "url": "https://svs.gsfc.nasa.gov/11497/", "result_type": "Produced Video", "release_date": "2014-02-28T11:30:00-05:00", "title": "Giant Sunspot Makes Third Trip Across the Sun", "description": "A giant sunspot – a magnetically strong and complex region on the sun's surface – has just appeared over the sun's horizon. This is the third trip for this region across the face of the sun, which takes approximately 27 days to make a complete rotation.Scientists track sunspots that are part of active regions, which often produce large explosions on the sun such as solar flares and coronal mass ejections, or CMEs. Each time an active region appears it is assigned a number. Active regions that have survived their trip around the back of the sun and reappear are assigned a new number – a convention left over from when we had no telescopes observing the far side of the sun and so could not be sure that the new sunspot was indeed the same as the old one. This active region is currently labeled AR11990. Last time around it was labeled AR11967and its first time it was AR11944.During its three trips thus far, this region has produced two significant solar flares, labeled as the strongest kind of flare, an X-class. It has also produced numerous mid-level and smaller flares. While many sunspots do not last more than a couple of weeks, there have been sunspots known to be stable for many months at a time.Studying what causes active regions to appear and disappear over time, as well as how long they remain stable, is key to understanding the origins of space weather that can impact Earth’s technological infrastructure. || ", "hits": 72 }, { "id": 11215, "url": "https://svs.gsfc.nasa.gov/11215/", "result_type": "Produced Video", "release_date": "2014-02-20T11:00:00-05:00", "title": "PSR J1311-3430 'Black Widow' Pulsar Animations", "description": "The essential features of black widow binaries, and their cousins, known as redbacks, are that they place a normal but very low-mass star in close proximity to a millisecond pulsar, which has disastrous consequences for the star. Black widow systems contain stars that are both physically smaller and of much lower mass than those found in redbacks.So far, astronomers have found at least 18 black widows and nine redbacks within the Milky Way, and additional members of each class have been discovered within the dense globular star clusters that orbit our galaxy. These animations show artist's impressions of one system, named PSR J1311-3430. Discovered in 2012, J1311 sets the record for the tightest orbit of its class and contains one of the heaviest neutron stars known. The pulsar's featherweight companion, which is only a dozen or so times the mass of Jupiter and just 60 percent of its size, completes an orbit every 93 minutes – less time than it takes to watch most movies. Recent studies allow a range of values extending down to 2 solar masses for the pulsar, still among the highest-known for neutron stars. || ", "hits": 267 }, { "id": 11136, "url": "https://svs.gsfc.nasa.gov/11136/", "result_type": "Produced Video", "release_date": "2014-01-07T16:00:00-05:00", "title": "Sun unleashes first X-class flare of 2014", "description": "The sun emitted a significant solar flare peaking at 1:32 p.m. EST on Jan.7, 2014. This is the first significant flare of 2014, and follows on the heels of mid-level flare earlier in the day. Each flare was centered over a different area of a large sunspot group currently situated at the center of the sun, about half way through its 14-day journey across the front of the disk along with the rotation of the sun. This flare is classified as an X1.2-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. || ", "hits": 79 }, { "id": 30467, "url": "https://svs.gsfc.nasa.gov/30467/", "result_type": "Hyperwall Visual", "release_date": "2013-11-01T12:00:00-04:00", "title": "Under the 'Wing\" of the Small Magellanic Cloud", "description": "The Small Magellanic Cloud (SMC) is one of the Milky Way's closest galactic neighbors. Even though it is a small, or so-called dwarf galaxy, the SMC is so bright that it is visible to the unaided eye from the Southern Hemisphere and near the equator. Many navigators, including Ferdinand Magellan who lends his name to the SMC, used it to help find their way across the oceans. NASA's Chandra X-ray telescope has made the first detection of X-ray emission from young solar-type stars—stars with characteristics broadly similar to those of our sun—that lie outside our Milky Way galaxy. These stars live in a region known as the \"Wing\" of the SMC. This image of the Wing is a composite that combines data from three sources into one. X-ray data from Chandra are shown in purple; optical (i.e., visible) light seen by the Hubble Space Telescope is in red, green, and blue; and infrared data from the Spitzer Space Telescope are colored red. X-rays from young stars trace the activity and strength of stellar magnetic fields. Magnetic activity provides clues to a star's convection (the rising and falling of hot gas in the star's interior) and rotation rates. The combined X-ray, optical, and infrared data also reveal, for the first time outside our galaxy, objects that resemble very young, lowmass stars, which scientists call \"young stellar objects.\" These objects have ages of a few thousand years and are still embedded in the pillar of dust and gas from which stars form.Used in 2014 Calendar. || ", "hits": 71 }, { "id": 30362, "url": "https://svs.gsfc.nasa.gov/30362/", "result_type": "Hyperwall Visual", "release_date": "2013-10-22T12:00:00-04:00", "title": "Full Map of the Sun's Surface", "description": "This movie shows the evolution of the Sun's entire surface as seen in extreme ultraviolet light (304 angstroms) for the time period Jan 1 - Sep 27, 2012. The movie was made by combining nearly simultaneous view of the Sun from three spacecraft: STEREO AHEAD and BEHIND (seeing the Sun's far side) and the Solar Dynamic Observer (seeing the near side). This EUV light comes primarily from the solar chromosphere. The bright patches are active regions. Many dark prominence eruptions can also be seen. The data is plotted in Carrington coordinates which are \"fixed\" to the surface of the Sun. In this coordinate system, the active regions tend to stay at the same location. However, the Sun's rotation rate actually changes with latitude and this can be seen in the movie. || ", "hits": 617 }, { "id": 11291, "url": "https://svs.gsfc.nasa.gov/11291/", "result_type": "Produced Video", "release_date": "2013-06-12T10:00:00-04:00", "title": "The Moon and the Sun: Two NASA Missions Join Their Images", "description": "Two or three times a year, NASA’s Solar Dynamics Observatory observes the moon traveling across the sun, blocking its view. While this obscures solar observations for a short while, it offers the chance for an interesting view of the shadow of the moon. The moon’s crisp horizon can be seen up against the sun, since the moon does not have an atmosphere. (At other times of the year, when Earth blocks SDO’s view, the Earth’s horizon looks fuzzy due to its atmosphere.) If one looks closely at such a crisp border, the features of the moon’s topography are visible, as is the case in this image from Oct. 7, 2010. This recently inspired two NASA visualizers to overlay a 3-dimensional model of the moon based on data from NASA’s Lunar Reconnaissance Orbiter into the shadow of the SDO image. Such a task is fairly tricky, as the visualizers — Scott Wiessinger who typically works with the SDO imagery and Ernie Wright who works with the LRO imagery — had to precisely match up data from the correct time and viewpoint for the two separate instruments. The end result is an awe-inspiring image of the sun and the moon. To start the process, the visualizers took the viewing position and time from the SDO image. This information was dropped into an LRO model that can produce the exact view of the moon from anywhere, at any time, by incorporating 6 billion individual measurements of the moon’s surface height from LRO’s Lunar Orbiter Laser Altimeter instrument. The model had to take many factors into consideration, including not only SDO’s distance and viewing angle, but also the moon’s rotation and constant motion. Wright used animation software to wrap the elevation and appearance map around a sphere to simulate the moon. The two images were put together and the overlay was exact. The mountains and valleys on the horizon of the LRO picture fit right into the shadows seen by SDO. In its own way, this served as a kind of calibration of data. It means that the SDO data on its position and time is highly accurate and that the LRO models, too, are able to accurately provide images of what’s happening at any given moment in time. And of course, the whole exercise provides for a beautiful picture. || ", "hits": 299 }, { "id": 11255, "url": "https://svs.gsfc.nasa.gov/11255/", "result_type": "Produced Video", "release_date": "2013-04-22T14:00:00-04:00", "title": "Three Years of SDO Images", "description": "In the three years since it first provided images of the sun in the spring of 2010, NASA's Solar Dynamics Observatory (SDO) has had virtually unbroken coverage of the sun's rise toward solar maximum, the peak of solar activity in its regular 11-year cycle. This video shows those three years of the sun at a pace of two images per day. Each image is displayed for two frames at a 29.97 frame rate.SDO's Atmospheric Imaging Assembly (AIA) captures a shot of the sun every 12 seconds in 10 different wavelengths. The images shown here are based on a wavelength of 171 angstroms, which is in the extreme ultraviolet range and shows solar material at around 600,000 Kelvin. In this wavelength it is easy to see the sun's 25-day rotation as well as how solar activity has increased over three years.During the course of the video, the sun subtly increases and decreases in apparent size. This is because the distance between the SDO spacecraft and the sun varies over time. The image is, however, remarkably consistent and stable despite the fact that SDO orbits the Earth at 6,876 miles per hour and the Earth orbits the sun at 67,062 miles per hour.Such stability is crucial for scientists, who use SDO to learn more about our closest star. These images have regularly caught solar flares and coronal mass ejections in the act, types of space weather that can send radiation and solar material toward Earth and interfere with satellites in space. SDO's glimpses into the violent dance on the sun help scientists understand what causes these giant explosions — with the hopes of some day improving our ability to predict this space weather.The four wavelength view at the end of the video shows light at 4500 angstroms, which is basically the visible light view of the sun, and reveals sunspots; light at 193 angstroms which highlights material at 1 million Kelvin and reveals more of the sun's corona; light at 304 angstroms which highlights material at around 50,000 Kelvin and shows features in the transition region and chromosphere of the sun; and light at 171 angstroms.Noteworthy events that appear briefly in the main sequence of this video:00:30;24 Partial eclipse by the moon00:31;16 Roll maneuver01:11;02 August 9, 2011 X6.9 Flare, currently the largest of this solar cycle01:28;07 Comet Lovejoy, December 15, 201101:42;29 Roll Maneuver01:51;07 Transit of Venus, June 5, 201202:28;13 Partial eclipse by the moonWatch this video on YouTube. || ", "hits": 188 }, { "id": 10960, "url": "https://svs.gsfc.nasa.gov/10960/", "result_type": "Produced Video", "release_date": "2013-02-01T00:00:00-05:00", "title": "OSIRIS-REx Animations", "description": "THIS PAGE FEATURES OLDER CONTENT FOR OSIRIS-REx. NEWER CONTENT IS AVAILABLE ON THE OSIRIS-REx GALLERY. || ", "hits": 83 }, { "id": 3990, "url": "https://svs.gsfc.nasa.gov/3990/", "result_type": "Visualization", "release_date": "2012-11-20T09:00:00-05:00", "title": "The Active Sun from SDO: HMI Dopplergram", "description": "The Solar Dynamics Observatory (SDO) observes the Sun with many different instruments, in many different wavelengths of light. Many of these capabilities are not possible for ground-based observatories - hence the need for a space-based observing platform.The Helioseismic Magnetic Imager (HMI) aboard the Solar Dynamics Observatory takes a series of images every 45 seconds in a very narrow range of wavelengths in visible light of the solar photosphere. The wavelengths correspond to a region around the 6173 Ångstroms (617.3 nanometers) spectral line of neutral iron (Fe I). From this series of images, it constructs a set of images which extract other characteristics of the photosphere. For this dataset, it measures the shifting of the spectral lines to determine the velocity of gas flows on the solar surface. This spectral line shift is due to the Doppler effect (Wikipedia). Blue represents motion towards the observer. Red indicates motion away from the observer. For the images below, the color is dominated by the solar rotation, so the solar limb on the right is moving away from us (and therefore red) while the left limb is moving towards us (and therefore blue). Motions on the solar surface generate the rippling in the color and you can see evidence of surface flows around the sunspot near the left limb. This visualization is one of a set of visualizations (others linked below) covering the same time span of 17 hours over the full wavelength range of the mission. They are setup to play synchronously on a Hyperwall, or can be run individually.The images are sampled every 36 seconds, 1/3 of the standard time-cadence for SDO. This visualization is useful for illustrating how different solar phenomena, such as sunspots and active regions, look very different in different wavelengths of light. These differences enable scientists to study them more completely, with an eventual goal of improving Space Weather forecasting. || ", "hits": 150 }, { "id": 4006, "url": "https://svs.gsfc.nasa.gov/4006/", "result_type": "Visualization", "release_date": "2012-10-31T00:00:00-04:00", "title": "The Radiation Belts as seen by SAMPEX", "description": "This is a simulation of the Earth's radiation belts constructed from SAMPEX data around the time of the 2003 Halloween solar storms. In this visualization, we present the belts in cross-section to provide a better view of their interior structure.The Earth's magnetosphere is a very large magnetic structure around the Earth, and gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, while they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the magnetic dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration (Wikipedia). In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field (Wikipedia). The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere.This dataset was also used to generate radiation belts for the RBSP prelaunch visualizations. || ", "hits": 98 }, { "id": 3949, "url": "https://svs.gsfc.nasa.gov/3949/", "result_type": "Visualization", "release_date": "2012-05-08T00:00:00-04:00", "title": "Earth's Radiation Belts (side view)", "description": "This is a simulation of the Earth's radiation belts. In this version, we've kept the belts full structure. There is also a cross-section view of the belts in Earth's Radiation Belts (cross-section).The Earth's magnetosphere is a very large magnetic structure around the Earth, which gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, which they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration. In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field. The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is time-shifted from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere. || ", "hits": 49 }, { "id": 3950, "url": "https://svs.gsfc.nasa.gov/3950/", "result_type": "Visualization", "release_date": "2012-05-01T00:00:00-04:00", "title": "Earth's Radiation Belts (cross-section)", "description": "This is a simulation of the Earth's radiation belts. In this version, we've 'sliced' the belts open to provide a better view of their structure in cross-section. The non-cross-section view of the belts is Earth's Radiation Belts (side view)The Earth's magnetosphere is a very large magnetic structure around the Earth, and gets stretched into a large, teardrop-shaped configuration through its interaction with the solar wind. A number of the magnetic field lines, while they may originate on the Earth, do not connect back to the Earth, but connect into the magnetic field carried by the solar wind. However, near the Earth, the dipole component of the field is stronger than the solar wind field, and this allows all the magnetic field lines to connect back to the Earth, forming (approximately) the classic magnetic dipole configuration. In this region, lower energy electrons and ions, many from the Earth's ionosphere, can become trapped by the magnetic field to form the radiation belts.The radiation belt model is constructed from particle flux information from the SAMPEX mission, with the flux mapped to constant L-shells of the Earth's dipole magnetic field. The model is anchored to the Earth's geomagnetic field axis, which is not perfectly aligned with the Earth's rotation axis. This creates a small wobble of the radiation belts with time, which can be seen in this visualization.The data driving the radiation belt structure is time-shifted from the 2003 Halloween solar storms, a series of strong solar eruptions that began in late October 2003 and continued into the first week of November. During this time, the particle content of the belts change rapidly due to the variation in the energetic particle flux from the Sun buffeting the Earth's magnetosphere. || ", "hits": 182 }, { "id": 3898, "url": "https://svs.gsfc.nasa.gov/3898/", "result_type": "Visualization", "release_date": "2012-01-27T00:00:00-05:00", "title": "Growing Sunspots - Tracking Closeup: February 2011", "description": "This visualization tracks the emergence and evolution of a sunspot group as seen by SDO/HMI starting in early February 2011 and continuing for two weeks. Images are sampled one hour apart.In this version, the camera tracks the movement of the solar rotation.At this scale, a 'shimmer' of the solar surface is visible, created by the turnover of convection cells. A higher-resolution view of these convection cells can be seen in Hinode imagery (see entry #3412, Hinode's High-resolution view of solar granulation).For a full-disk view of the Sun, covering the same time frame, see entry #3897, Growing Sunspots - A Full Disk View: February 2011. || ", "hits": 21 }, { "id": 3828, "url": "https://svs.gsfc.nasa.gov/3828/", "result_type": "Visualization", "release_date": "2011-12-07T00:00:00-05:00", "title": "Solar Dynamics Observatory - Atmospheric Imaging Assembly", "description": "The Sun's activity increases as we enter solar cycle 24. But even several years away from the peak, the Sun in ultraviolet light shows a variety of activity.This visualization consists of eight hours of SDO AIA imagery from the 30.4 nanometer filter (304 Ångstroms). This sequence plays at the full time cadence of the AIA instrument - one image every twelve seconds of real time - and showing thirty images per second on playback. || ", "hits": 165 }, { "id": 40115, "url": "https://svs.gsfc.nasa.gov/gallery/space-weather/", "result_type": "Gallery", "release_date": "2011-12-01T00:00:00-05:00", "title": "Space Weather", "description": "The term \"space weather\" was coined not long ago to describe the dynamic conditions in the Earth's outer space environment, in the same way that \"weather\" and \"climate\" refer to conditions in Earth's lower atmosphere. Space weather includes any and all conditions and events on the sun, in the solar wind, in near-Earth space and in our upper atmosphere that can affect space-borne and ground-based technological systems and through these, human life and endeavor. Heliophysics is the science of space weather.\r\n\r\nThis gallery organizes satellite footage, animations, visualizations, and edited videos produced at the Goddard Space Flight Center. Visualizations are different from pure animations because they are data-driven. They present a way of \"seeing\" the data. In the case of orbit visualizations, they are based on actual orbit information. Most of the animations and visualizations are available as frames and all the recent ones are HD quality. All videos are available in several formats and qualities including Apple ProRes for broadcast quality. Unless specifically marked otherwise, all these materials are public domain and free to use. For more infomation about NASA's media use guidelines see this page.\r\n\r\nThe content is organized in two ways. Under \"Facets of Space Weather\" you will find our visuals grouped by the subject they address. Under \"NASA Spacecraft\" you will find our visuals grouped by the satellite they were collected by, or that they refer to. This group also contains animations of the spacecraft themselves.\r\nFor breaking news solar events, go to this gallery.For frequently-asked-question interviews with NASA scientists, go here.", "hits": 113 }, { "id": 10817, "url": "https://svs.gsfc.nasa.gov/10817/", "result_type": "Produced Video", "release_date": "2011-09-07T12:00:00-04:00", "title": "SDO EVE Late Phase Flares", "description": "Scientists have been seeing just the tip of the iceberg when monitoring flares with X-rays. With the complete extreme ultraviolet (EUV) coverage by the SDO EUV Variability Experiment (EVE), they have observed enhanced EUV radiation that appears not only during the X-ray flare, but also a second time delayed by many minutes after the X-ray flare peak. These delayed, second peaks are referred to as the EUV Late Phase contribution to flares.The solar EUV radiation creates our Earth's ionosphere (plasma in our atmosphere), so solar flares disturb our ionosphere and consequently our communication and navigation technologies, such as Global Positioning System (GPS), that transmit through the ionosphere. For over 30 years, scientists have relied on the GOES X-ray monitor to tell them when to expect disturbances to our ionosphere. With these new SDO EVE results, they now recognize that additional ionospheric disturbances from these later EUV enhancements are also a concern. || ", "hits": 75 }, { "id": 10790, "url": "https://svs.gsfc.nasa.gov/10790/", "result_type": "Produced Video", "release_date": "2011-06-09T12:00:00-04:00", "title": "Voyager Satellites Find Magnetic Bubbles at Edge of Solar System", "description": "The sun's magnetic field spins opposite directions on the north and south poles. These oppositely pointing magnetic fields are separated by a layer of current called the heliospheric current sheet. Due to the tilt of the magnetic axis in relation to the axis of rotation of the Sun, the heliospheric current sheet flaps like a flag in the wind. The flapping current sheet separates regions of oppositely pointing magnetic field, called sectors. As the solar wind speed decreases past the termination shock, the sectors squeeze together, bringing regions of opposite magnetic field closer to each other. The Voyager spacecraft have now found that when the separation of sectors becomes very small, the sectored magnetic field breaks up into a sea of nested \"magnetic bubbles\" in a phenomenon called magnetic reconnection. The region of nested bubbles is carried by the solar wind to the north and south filling out the entire front region of the heliopause and the sector region in the heliosheath.This discovery has prompted a complete revision of what the heliosheath region looks like. The smooth, streamlined look is gone, replaced with a bubbly, frothy outer layer. More animations about the Voyager magnetic bubbles discovery are available. || ", "hits": 169 }, { "id": 10791, "url": "https://svs.gsfc.nasa.gov/10791/", "result_type": "Produced Video", "release_date": "2011-06-09T12:00:00-04:00", "title": "Voyager Heliosheath Bubbles Animations", "description": "Animations showing the new Voyager findings about the magnetic field in the heliosheath.For more videos and stills about the Voyager magnetic bubbles discovery, go here. || ", "hits": 118 }, { "id": 10767, "url": "https://svs.gsfc.nasa.gov/10767/", "result_type": "Produced Video", "release_date": "2011-05-11T12:00:00-04:00", "title": "NASA's Fermi Spots 'Superflares' in the Crab Nebula", "description": "The famous Crab Nebula supernova remnant has erupted in an enormous flare five times more powerful than any previously seen from the object. The outburst was first detected by NASA's Fermi Gamma-ray Space Telescope on April 12 and lasted six days.The nebula, which is the wreckage of an exploded star whose light reached Earth in 1054, is one of the most studied objects in the sky. At the heart of an expanding gas cloud lies what's left of the original star's core, a superdense neutron star that spins 30 times a second. With each rotation, the star swings intense beams of radiation toward Earth, creating the pulsed emission characteristic of spinning neutron stars (also known as pulsars). Apart from these pulses, astrophysicists regarded the Crab Nebula to be a virtually constant source of high-energy radiation. But in January, scientists associated with several orbiting observatories — including NASA's Fermi, Swift and Rossi X-ray Timing Explorer — reported long-term brightness changes at X-ray energies.Scientists think that the flares occur as the intense magnetic field near the pulsar undergoes sudden restructuring. Such changes can accelerate particles like electrons to velocities near the speed of light. As these high-speed electrons interact with the magnetic field, they emit gamma rays in a process known as synchrotron emission.To account for the observed emission, scientists say that the electrons must have energies 100 times greater than can be achieved in any particle accelerator on Earth. This makes them the highest-energy electrons known to be associated with any cosmic source.Based on the rise and fall of gamma rays during the April outbursts, scientists estimate that the size of the emitting region must be comparable in size to the solar system. If circular, the region must be smaller than roughly twice Pluto's average distance from the sun.For more Crab Nebula media go to #10708. || ", "hits": 60 }, { "id": 10623, "url": "https://svs.gsfc.nasa.gov/10623/", "result_type": "Produced Video", "release_date": "2010-07-29T00:00:00-04:00", "title": "Rebounding Plasma Flows in the Inner Magnetosphere", "description": "Substorms send jets of plasma careening Earthward at speeds near 600,000 miles/hour. Researchers comparing multipoint THEMIS spacecraft observations with the predictions of numerical simulations have determined the width of one such jet and determined what happened to it when it encountered the strong magnetic fields within the inner magnetosphere. Plasma jets with the width of the Earth slam into the inner magnetosphere, generating vortices with opposite senses of rotation that appear and disappear on either side of the plasma jet. These vortices become sources of field-aligned electrical currents that flow down to the Earth's ionosphere, where they generate auroral brightenings and intense magnetic field disturbances. After striking the inner magnetospheric magnetic field, the plasma jet itself bounces back and forth, losing energy each time it encounters the magnetic field, and continuing to oscillate until the flow energy is dissipated in the form of plasma heating. || ", "hits": 58 }, { "id": 10595, "url": "https://svs.gsfc.nasa.gov/10595/", "result_type": "Produced Video", "release_date": "2010-06-23T00:00:00-04:00", "title": "Ten Cool Things Seen in the First Year of LRO", "description": "Having officially reached lunar orbit on June 23nd, 2009, the Lunar Reconnaissance Orbiter (LRO) has now marked one full year on its mission to scout the moon. Maps and datasets collected by LRO's state-of-the-art instruments will form the foundation for all future lunar exploration plans, as well as be critical to scientists working to better understand the moon and its environment. In only the first year of the mission, LRO has gathered more digital information than any previous planetary mission in history. To celebrate one year in orbit, here are ten cool things already observed by LRO. Note that the stories here are just a small sample of what the LRO team has released and barely touch on the major scientific accomplishments of the mission. If you like these, visit the official LRO web site at www.nasa.gov/LRO to find out even more! || ", "hits": 588 } ] }