{ "count": 81, "next": null, "previous": null, "results": [ { "id": 14707, "url": "https://svs.gsfc.nasa.gov/14707/", "result_type": "Produced Video", "release_date": "2024-11-25T11:00:00-05:00", "title": "XRISM's Resolve Instrument Gazes into Cygnus X-3", "description": "Cygnus X-3 is a high-mass X-ray binary system consisting of a compact object (likely a black hole) and a Wolf-Rayet star. This artist's concept shows one interpretation of the system. High-resolution X-ray spectroscopy indicates two gas components: a heavy background outflow, or wind, produced by the massive star and a turbulent structure — perhaps a wake carved into the wind — located close to the orbiting companion. As shown here, a black hole's gravity captures some of the wind into an accretion disk around it, and the disk's orbital motion sculpts a path (yellow arc) through the streaming gas. During strong outbursts, the companion emits jets of particles moving near the speed of light, seen here extending above and below the black hole.Credit: NASA’s Goddard Space Flight CenterAlt text: Illustration of the Cygnus X-3 systemImage description: On a cloudy reddish background, a bright blue-white circle — a representation of a hot, bright, massive star — sits near the center. Wisps of blue-white border its edges, and many lines of similar color radiate from it. In the foreground at about 4 o’clock lies a yellowish ring with a black hole in its center. From the ring trails a diffuse yellow arc, sweeping from right to left and exiting at the bottom of the illustration. Extending above and below the black hole are two blue-white triangles representing particle jets. || Cyg_X-3_illustration_4K.jpg (3840x2160) [505.1 KB] || Cyg_X-3_illustration_4K_print.jpg (1024x576) [58.5 KB] || Cyg_X-3_illustration_4K_searchweb.png (320x180) [64.7 KB] || Cyg_X-3_illustration_4K_web.png (320x180) [64.7 KB] || Cyg_X-3_illustration_4K_thm.png (80x40) [6.1 KB] || ", "hits": 597 }, { "id": 5333, "url": "https://svs.gsfc.nasa.gov/5333/", "result_type": "Visualization", "release_date": "2024-10-07T09:00:00-04:00", "title": "DYAMOND Global Carbon Dioxide for Fulldome", "description": "Global CO2 ppm for January-March of 2020. This camera move orbits the Earth from a distance. || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k.00200_print.jpg (1024x1024) [19.8 KB] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k.00200_searchweb.png (320x180) [5.4 KB] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k.00200_web.png (320x320) [6.0 KB] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k.00200_thm.png (80x40) [751 bytes] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome_2048p30_h264.mp4 (2048x2048) [2.2 MB] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k [0 Item(s)] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k_4096p30_h265.mp4 (4096x4096) [9.0 MB] || dyamondPointCloud_12-4-2023b_dyamond_co2_anim_globe_orbit_dome4k_4096p30_h265.mp4.hwshow || ", "hits": 158 }, { "id": 5196, "url": "https://svs.gsfc.nasa.gov/5196/", "result_type": "Visualization", "release_date": "2024-07-22T09:00:00-04:00", "title": "DYAMOND Global Carbon Dioxide", "description": "Global CO2 ppm for January-March of 2020. This camera move orbits the Earth from a distance. || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_3x3Hyperwall.00200_print.jpg (1024x576) [46.2 KB] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_3x3Hyperwall.00200_searchweb.png (320x180) [31.3 KB] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_3x3Hyperwall.00200_web.png (320x180) [31.3 KB] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_3x3Hyperwall.00200_thm.png (80x40) [3.0 KB] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_1080p30_h265.mp4 (1920x1080) [6.9 MB] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_3x3Hyperwall (5760x3240) [0 Item(s)] || dyamondPointCloud_12-1-2023b_dyamond_co2_anim_globe_orbit_2160p30.mp4 (3840x2160) [68.4 MB] || ", "hits": 429 }, { "id": 14584, "url": "https://svs.gsfc.nasa.gov/14584/", "result_type": "Produced Video", "release_date": "2024-05-08T09:00:00-04:00", "title": "XRISM Spots Iron Fingerprints in Nearby Active Galaxy", "description": "The Resolve instrument aboard XRISM (X-ray Imaging and Spectroscopy Mission) captured data from the center of galaxy NGC 4151, where a supermassive black hole is slowly consuming material from the surrounding accretion disk. The resulting spectrum reveals the presence of iron in the peak around 6.5 keV and the dips around 7 keV, light thousands of times more energetic that what our eyes can see. Background: An image of NGC 4151 constructed from a combination of X-ray, optical, and radio light. Credit: Spectrum: JAXA/NASA/XRISM Resolve. Background: X-rays, NASA/CXC/CfA/J.Wang et al.; optical, Isaac Newton Group of Telescopes, La Palma/Jacobus Kapteyn Telescope; radio, NSF/NRAO/VLAAlt text: A XRISM spectrum of NGC 4151 with a multiwavelength snapshot of the galaxy in the background. Descriptive text: The spectrum image is labeled, “XRISM Resolve Spectrum of NGC 4151.” It shows a graph where the bottom is labeled, “X-ray energy (keV),” with a range from 5 to 9. The left side is labeled, “X-ray brightness.” A squiggly white line starts just under halfway up the left side. It peaks at just under 6.5 keV, nearly reaching the top of the graph. Then it starts to slope gently downward, with several sharp dips around 7 keV. In the background is a dim image of galaxy NGC 4151, where the center is a whiteish blue, surrounding by clouds of red and yellow. || Spectrum_v4.jpg (2300x2050) [426.6 KB] || ", "hits": 132 }, { "id": 5273, "url": "https://svs.gsfc.nasa.gov/5273/", "result_type": "Visualization", "release_date": "2024-04-22T00:00:00-04:00", "title": "Atmospheric Carbon Dioxide Tagged by Source for Science-on-a-Sphere", "description": "Carbon dioxide (CO2) is the most prevalent greenhouse gas driving global climate change. However, its increase in the atmosphere would be even more rapid without land and ocean carbon sinks, which collectively absorb about half of human emissions every year. Advanced computer modeling techniques in NASA's Global Modeling and Assimilation Office allow us to disentangle the influences of sources and sinks and to better understand where carbon is coming from and going to.", "hits": 175 }, { "id": 31248, "url": "https://svs.gsfc.nasa.gov/31248/", "result_type": "Hyperwall Visual", "release_date": "2023-09-29T00:00:00-04:00", "title": "How Do Space Weather Effects & Solar Storms Affect Earth?", "description": "Technological and infrastructure affected by space weather events. || space-weather-effects_print.jpg (1024x953) [307.6 KB] || space-weather-effects.png (3480x3240) [8.3 MB] || space-weather-effects_searchweb.png (320x180) [77.3 KB] || space-weather-effects_thm.png (80x40) [6.2 KB] || how-do-space-weather-effects-solar-storms-affect-earth.hwshow [320 bytes] || ", "hits": 431 }, { "id": 5110, "url": "https://svs.gsfc.nasa.gov/5110/", "result_type": "Visualization", "release_date": "2023-06-16T10:00:00-04:00", "title": "Atmospheric Carbon Dioxide Tagged by Source", "description": "Carbon dioxide (CO2) is the most prevalent greenhouse gas driving global climate change. However, its increase in the atmosphere would be even more rapid without land and ocean carbon sinks, which collectively absorb about half of human emissions every year. Advanced computer modeling techniques in NASA's Global Modeling and Assimilation Office allow us to disentangle the influences of sources and sinks and to better understand where carbon is coming from and going to. ||", "hits": 1131 }, { "id": 40479, "url": "https://svs.gsfc.nasa.gov/gallery/carbon-dioxide-sources-sinks/", "result_type": "Gallery", "release_date": "2023-06-07T00:00:00-04:00", "title": "Carbon Dioxide Sources and Sinks", "description": "NASA models the flow of carbon dioxide; its emission, its transport around the globe, and its absorption by the ocean and biosphere.\n\n", "hits": 107 }, { "id": 5047, "url": "https://svs.gsfc.nasa.gov/5047/", "result_type": "Visualization", "release_date": "2022-11-30T00:00:00-05:00", "title": "Net Ecosystem Exchange of Carbon Dioxide", "description": "The NASA Carbon Monotoring System's estimate of the Net Ecosystem Exchange of Carbon Dioxide from 2000 to 2018. || co2_nee_5.01750_print.jpg (1024x576) [124.3 KB] || co2_nee_5.01750_searchweb.png (320x180) [43.8 KB] || co2_nee_5.01750_thm.png (80x40) [4.5 KB] || 3840x2160_16x9_30p (3840x2160) [64.0 KB] || co2_nee_5.webm (3840x2160) [14.2 MB] || co2_nee_5.mp4 (3840x2160) [256.2 MB] || ", "hits": 352 }, { "id": 13983, "url": "https://svs.gsfc.nasa.gov/13983/", "result_type": "Produced Video", "release_date": "2021-11-01T09:55:00-04:00", "title": "Hubble's Field Guide to Nebulae", "description": "Nebulae are some of the most resplendent objects in the universe, but it’s easy to confuse which one is an “emission nebula,” and which one is an “absorption nebula.” Thankfully, this “Field Guide” will give you a quick rundown so you can impress all of your friends with your Nebulae Knowledge! And thanks to the Hubble Space Telescope, we can study all sorts of nebulae in all of their magnificent forms. For more information, visit https://nasa.gov/hubble. Additional Credits:Photo Logo Opener by Tony Ivonin via Motion ArrayMusic Credits: “Himalayan Temple” by Jan Pham Huu Tri [SACEM] via Koka Media [SACEM], Universal Production Music France [SACEM], and Universal Production Music || ", "hits": 85 }, { "id": 20340, "url": "https://svs.gsfc.nasa.gov/20340/", "result_type": "Animation", "release_date": "2021-03-22T11:00:00-04:00", "title": "Landsat 9 Atmospheric Correction", "description": "Landsat collects light in visible and infrared wavelengths. Sunlight reflects off Earth’s surface, and scientists identify the land cover based on which wavelengths are reflected strongly or weakly.But sunlight is also reflected by particles in the atmosphere, which distorts the data and can lead to what looks like a haze in the imagery. Using basic principles of physics, and knowing the meteorological conditions, scientists can determine the effects of the scattering and absorption as light passes through the atmosphere. This atmospheric correction is essential to determining exactly how much of each wavelength reflected of the features of the surface, and having quantifiable data.The videos below show different examples of atmospheric scattering which need to be accounted for when doing atmospheric correction of satellite data. In these cases, it is for observations over water. The resulting atmospheric corrections are part of the process for the new Landsat Aquatic Reflectance data product. Landsat’s highly calibrated data products, free to download and use, are making detailed Earth-observation data more accessible to users and bringing a greater benefit to society. || ", "hits": 63 }, { "id": 13680, "url": "https://svs.gsfc.nasa.gov/13680/", "result_type": "Produced Video", "release_date": "2020-08-06T09:55:00-04:00", "title": "Hubble Views the Moon to Study Earth", "description": "Taking advantage of the total lunar eclipse of January 2019, astronomers, using NASA’s Hubble Space Telescope, have measured the amount of ozone in the Earth’s atmosphere. The method used serves as a proxy for how they will observe earthlike planets around other stars in search for worlds similar to our own.For more information, visit https://nasa.gov/hubble.Visualizations:NASA/GSFC: K. Kim — Moonbounce AnimationESA, NASA and L. Calçada (ESO) — Artist's concept of exoplanet orbiting FomalhautESA, Hubble, M. Kornmesser —Absorption Lines & ExoplanetsNASA/GSFC: Chris Smith — TOI 700 system transit Animation ESA, Hubble, M. Kornmesser & L. L. Christensen — HD 189733b transiting its parent star (artist's impression) ESA, ESO/L. Calçada, M. Kornmesser & L. L. Christensen (ESA/Hubble) — Exoplanet Transit MethodVideos & Images: NASA Goddard Space Flight Center European Space AgencySpace Telescope Science InstituteJanuary 2019 Moon Image taken by Kevin HartnettArtbeats Stock Footage — Footage of leafPond5 Stock Footage — Footage of weeping willowfootagefirm — Footage of sunrise and cloudsMusic Credits:“Life Unplanned” by Paul Saunderson [ PRS ]. Abbey Road Masters [ PRS ], and Universal Production Music || ", "hits": 46 }, { "id": 13114, "url": "https://svs.gsfc.nasa.gov/13114/", "result_type": "Produced Video", "release_date": "2018-12-17T10:00:00-05:00", "title": "GEDI Overview", "description": "The GEDI instrument was built at NASA's Goddard Space Flight Center, and has the highest resolution and densest sampling of any lidar every put in orbit. The mission is led by the University of Maryland and is designed to help researchers understand how ecosystems are storing carbon.Complete transcript available.Music: Secret Science, by Lee Groves [PRS], Peter George Marett [PRS]; Team Effort, by Alexandre Prodhomme [SACEM], Eddy Pradelles [SACEM]Watch this video on the NASA Goddard YouTube channel. || GEDI_on_ISS_print.jpg (1024x576) [60.9 KB] || GEDI_on_ISS.png (3840x2160) [5.6 MB] || GEDI_on_ISS_searchweb.png (320x180) [56.5 KB] || GEDI_on_ISS_thm.png (80x40) [5.2 KB] || 13114_GEDI_overview_prores.mov (1920x1080) [6.3 GB] || 13114_GEDI_overview_youtube_1080.mp4 (1920x1080) [354.2 MB] || 13114_GEDI_overview_youtube_720.mp4 (1280x720) [354.4 MB] || 13114_GEDI_overview_twitter_720.mp4 (1280x720) [49.8 MB] || 13114_GEDI_overview.webm (960x540) [91.1 MB] || 13114_GEDI_overview-captions.en_US.srt [5.0 KB] || 13114_GEDI_overview-captions.en_US.vtt [5.0 KB] || ", "hits": 155 }, { "id": 13083, "url": "https://svs.gsfc.nasa.gov/13083/", "result_type": "Produced Video", "release_date": "2018-10-04T11:00:00-04:00", "title": "Hubble Archive - Post-Deployment", "description": "Digitized tape of the press conference from June 27, 1990 where Ed Weiler and others explain the Hubble Space Telescope's spherical aberration problem and its impact to the science instruments. The aberration wouldn't much affect UV or IR observations, but the Wide Field Planetary Camera would be largely affected since it used visible wavelengths. TRT: 30:00Participants: Douglas Broome, HST Program Manager; Jean Olivier, Deputy Project Manager; Dr. Edward Weiler, HST Program Scientist at NASA HQ; Dr. Lennard A. Fisk, Associate Administrator Space Science and Applications at NASA HQ; Dr. Peter Stockman, Deputy Director of the Space Telescope Science InstituteLonger notes:Describing the initial spherical aberration problem with the Hubble Space Telescope’s primary mirror. Describe how they conclusively determined the nature of the problem. It affects one of their science objectives. Weiler: “We can still do important science.” UV capability and IR capability not impacted. Spatial resolution is about at ground-based resolution. Explains impacts to each of the instruments. HRS - will be able to do most of the science, just not in crowded fields, still excellent for planetary features, least impacted instrument FOS - UV science not impacted except on crowded fields, quasar absorption lines won’t be impacted because point sources, FOC - highest spatial resolution of the cameras, visible wavelengths will be ground-based resolution except maybe better for bright objects, HSP - won’t be able to do science with high signal to noise, but can do about half of proposed science esp in UV WFPC - probably no real science we can do with this because in visible Fine guidance sensors for astrometry - can do 100% of science we proposed, will be able to look at star’s wobble to find exoplanetsBiggest impact is loss of spatial resolution for WFPCInsurance policy - planned for maintenance program, are already building a second wide-field camera with a corrective mirror, think we can take out all the aberration and get back to original specification, 40% of science was going to be done with wide-field camera, developing NICMOS for near-IR capability that includes corrective opticsFor HRS and FOS, have STIS under development which would replace spectrographic capabilities Haven’t yet figured out how the problem occured; putting together a review boardDon’t know if the aberration is in the primary or secondary mirrorDidn’t test the two mirrors in combination because it would have been tremendously costly and difficult (hundreds of millions of dollars)Cuts off at endAudio missing from 11:10 - 11:20 || GSFC_19900627_HST_m001_thumbnail.jpg (720x484) [131.8 KB] || GSFC_19900627_HST_m001_thumbnail_searchweb.png (320x180) [145.5 KB] || GSFC_19900627_HST_m001_thumbnail_thm.png (80x40) [9.4 KB] || GSFC_19900627_HST_m001.mov (720x486) [12.5 GB] || GSFC_19900627_HST_m001.mp4 (720x484) [2.1 GB] || GSFC_19900627_HST_m001.webm [0 bytes] || ", "hits": 57 }, { "id": 13032, "url": "https://svs.gsfc.nasa.gov/13032/", "result_type": "Produced Video", "release_date": "2018-08-08T11:00:00-04:00", "title": "Two Research Vessels Leave for the Twilight Zone", "description": "A project jointly funded by NASA and the National Science Foundation is heading west from Seattle, straight for the twilight zone. Using two research vessels, the Export Processes in the Ocean from Remote Sensing (EXPORTS) oceanographic campaign will study the fates and carbon cycle impacts of microscopic underwater organisms.The large multidisciplinary team, including members from more than 20 different research institutions, is accompanied by advanced underwater robotics and other instruments on a month-long campaign to study the secret lives of tiny organisms called phytoplankton, and the animals that eat them. These organisms can have a large impact on Earth's carbon cycle, storing carbon dioxide in a part of the ocean known as the twilight zone, between 650 and 3300 feet below the surface. || ", "hits": 24 }, { "id": 30950, "url": "https://svs.gsfc.nasa.gov/30950/", "result_type": "Hyperwall Visual", "release_date": "2018-05-15T16:00:00-04:00", "title": "Spiral Galaxy Pair NGC 4302 and NGC 4298 from Hubble", "description": "Spiral galaxies NGC 4302 and NGC 498 are similar in shape, but appear different due to their different observed orientations. || ngc4302_ngc4298-hst-6576x7614_print.jpg (1024x1185) [166.6 KB] || ngc4302_ngc4298-hst-6576x7614.png (6576x7614) [84.3 MB] || ngc4302_ngc4298-hst-6576x7614_searchweb.png (320x180) [81.9 KB] || ngc4302_ngc4298-hst-6576x7614_thm.png (80x40) [5.4 KB] || spiral-galaxy-pair-ngc-4302-and-ngc-4298-from-hubble.hwshow [249 bytes] || ", "hits": 100 }, { "id": 12850, "url": "https://svs.gsfc.nasa.gov/12850/", "result_type": "Produced Video", "release_date": "2018-03-28T13:00:00-04:00", "title": "NASA's New Planet Hunter: TESS", "description": "Watch an overview of the TESS mission.Music: \"Drive to Succeed\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || TESS_Still_B1_00812_print.jpg (1024x576) [56.9 KB] || TESS_Still_B1_00812.png (3840x2160) [5.6 MB] || TESS_Still_B1_00812_searchweb.png (320x180) [53.1 KB] || TESS_Still_B1_00812_thm.png (80x40) [4.8 KB] || 12850_TESS_Overview_1080.webm (1920x1080) [34.9 MB] || 12850_TESS_Overview_1080.m4v (1920x1080) [321.6 MB] || TESS_Overview_SRT_Captions.en_US.srt [5.8 KB] || TESS_Overview_SRT_Captions.en_US.vtt [5.8 KB] || 12850_TESS_Overview_4K_Good_H264.mov (3840x2160) [931.4 MB] || 12850_TESS_Overview_4K_Best_H264.m4v (3840x2160) [1.5 GB] || 12850_TESS_Overview.mp4 (3840x2160) [1.6 GB] || 12850_TESS_Overview_YOUTUBE.mov (3840x2160) [3.2 GB] || 12850_TESS_Overview_Prores_3840x2160_2997.mov (3840x2160) [17.2 GB] || ", "hits": 227 }, { "id": 12746, "url": "https://svs.gsfc.nasa.gov/12746/", "result_type": "Produced Video", "release_date": "2017-10-18T08:00:00-04:00", "title": "What Lurks Beneath NASA's Chamber A", "description": "Produced video about a new NASA molecular contamination control technology developed by Nithin Abraham, a coatings engineer at NASA's Goddard Space Flight Center in Greenbelt, Maryland. Nithin Abraham is part of a contamination control team tasked with ensuring Webb remains as clean as possible during its testing in Chamber A. Abraham developed and tested a highly permeable and porous material called molecular adsorber coating (MAC), which can be sprayed onto surfaces to passively capture contaminants that could be harmful to Webb's optics and science instruments. || MAC_Panels_IMAGE_ONLY1.00000_print.jpg (1024x576) [79.5 KB] || MAC_Panels_IMAGE_ONLY1.00000_searchweb.png (180x320) [76.5 KB] || MAC_Panels_IMAGE_ONLY1.00000_thm.png (80x40) [6.1 KB] || MAC_Panels_and_Plenum_ContaminationV4-ProRes.mov (1920x1080) [2.5 GB] || MAC_Panels_Plenum_Contamination-h264.mp4 (1920x1080) [194.3 MB] || MAC_Panels_Plenum_Contamination-h264.webm (1920x1080) [21.5 MB] || MAC_Panels_Plenum_Contamination-SRT-caption.en_US.srt [3.9 KB] || MAC_Panels_Plenum_Contamination-SRT-caption.en_US.vtt [3.9 KB] || ", "hits": 37 }, { "id": 4575, "url": "https://svs.gsfc.nasa.gov/4575/", "result_type": "Visualization", "release_date": "2017-07-31T00:00:00-04:00", "title": "NASA Studies Hurricane Matthew", "description": "This data visualization follows Hurricane Matthew throughout its destructive run in the Caribbean and Southeast U.S. coast. By utilizing different data sets from NOAA's GOES satellite, NASA/JAXA's GPM, MERRA-2 model runs, IMERG, Goddard's soil moisture product, and sea surface temperatures, scientists are able to put together a clearer picture of how this hurricane quickly intensified and eventually weakened. || matthew_narrated_v106.5800_print.jpg (1024x576) [189.6 KB] || matthew_narrated_v106.5800_searchweb.png (320x180) [114.8 KB] || matthew_narrated_v106.5800_thm.png (80x40) [7.8 KB] || matthew (1920x1080) [0 Item(s)] || matthew_narrated_v106.webm (1920x1080) [22.0 MB] || matthew_narrated_v106.mp4 (1920x1080) [140.5 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || matthew_narrated_v106_4k.mp4 (3840x2160) [443.1 MB] || matthew_narrated_nosound.hwshow || ", "hits": 47 }, { "id": 12629, "url": "https://svs.gsfc.nasa.gov/12629/", "result_type": "Produced Video", "release_date": "2017-06-09T12:00:00-04:00", "title": "Ocean Circulation Plays an Important Role in Absorbing Carbon from the Atmosphere", "description": "Music: Anywhere by François Pavan [SACEM], Mi-Yung Pavan [SACEM]Complete transcript available. || LARGE_MP4-12629_AMOCcarbon_large.00001_print.jpg (1024x576) [184.7 KB] || LARGE_MP4-12629_AMOCcarbon_large.00001_searchweb.png (320x180) [106.8 KB] || LARGE_MP4-12629_AMOCcarbon_large.00001_thm.png (80x40) [7.3 KB] || LARGE_MP4-12629_AMOCcarbon_large.mp4 (1920x1080) [51.2 MB] || WEBM-12629_AMOCcarbon.webm (960x540) [20.0 MB] || NASA_TV-12629_AMOCcarbon.mpeg (1280x720) [169.5 MB] || APPLE_TV-12629_AMOCcarbon_appletv.m4v (1280x720) [23.4 MB] || APPLE_TV-12629_AMOCcarbon_appletv_subtitles.m4v (1280x720) [23.4 MB] || 12629_AMOCcarbon.en_US.srt [819 bytes] || 12629_AMOCcarbon.en_US.vtt [832 bytes] || NASA_PODCAST-12629_AMOCcarbon_ipod_sm.mp4 (320x240) [8.5 MB] || ", "hits": 355 }, { "id": 12302, "url": "https://svs.gsfc.nasa.gov/12302/", "result_type": "Produced Video", "release_date": "2016-07-13T00:00:00-04:00", "title": "Aerosol Optical Thickness, MODIS, 2000-2016", "description": "Aerosol optical depth from Terra/MODIS, 1-month composite.In the maps shown here, dark brown pixels show high aerosol concentrations, while tan pixels show lower concentrations, and light yellow areas show little or no aerosols. Black shows where the sensor could not make its measurement.Aerosol optical depth is the degree to which aerosols prevent the transmission of light by absorption or scattering of light. || MODIS_Aerosol_Optical_Depth_youtube_hq.00001_print.jpg (1024x512) [184.9 KB] || MODIS_Aerosol_Optical_Depth_youtube_hq.00001_searchweb.png (320x180) [92.7 KB] || MODIS_Aerosol_Optical_Depth_youtube_hq.00001_thm.png (80x40) [6.7 KB] || MODIS_Aerosol_Optical_Depth.webm (960x540) [42.2 MB] || 3600x1800_2x1_30p (3600x1800) [16.0 KB] || GSFC_20160713_MODIS_m12302_Aerosol.en_US.vtt [64 bytes] || MODIS_Aerosol_Optical_Depth_large.mp4 (3600x1800) [233.1 MB] || MODIS_Aerosol_Optical_Depth_youtube_hq.mov (3600x1800) [511.0 MB] || MODIS_Aerosol_Optical_Depth_prores720.mov (1280x720) [1.7 GB] || MODIS_Aerosol_Optical_Depth_prores.mov (3600x1800) [11.1 GB] || ", "hits": 62 }, { "id": 12064, "url": "https://svs.gsfc.nasa.gov/12064/", "result_type": "Produced Video", "release_date": "2015-11-18T10:00:00-05:00", "title": "George Hurtt: Carbon and Climate Soundbite", "description": "George Hurtt, professor at University of Maryland, gives information on NASA's Carbon Monitoring System in advance of the United Nations COP-21 climate meeting in Paris, 2015For complete transcript, click here.Music credit: Rippling Rays by Jon Wygens || George_Hurtt_Cover_Image_print.jpg (1024x576) [72.6 KB] || George_Hurtt_Cover_Image_searchweb.png (320x180) [73.5 KB] || George_Hurtt_Cover_Image_thm.png (80x40) [4.8 KB] || George_Hurtt_MASTER_prores.mov (1280x720) [603.3 MB] || George_Hurtt_MASTER_youtube_hq.mov (1280x720) [147.2 MB] || George_Hurtt_MASTER_appletv.m4v (1280x720) [21.4 MB] || George_Hurtt_Carbon_Climate.mp4 (1280x720) [42.5 MB] || George_Hurtt_MASTER.mpeg (1280x720) [144.3 MB] || George_Hurtt_MASTER.webm (960x540) [17.2 MB] || George_Hurtt_Cover_Image.tif (1280x720) [3.5 MB] || George_Hurtt_MASTER_appletv_subtitles.m4v (1280x720) [21.5 MB] || 12064_George_Hurtt_captions.en_US.srt [972 bytes] || 12064_George_Hurtt_captions.en_US.vtt [979 bytes] || George_Hurtt_MASTER_ipod_sm.mp4 (320x240) [7.6 MB] || ", "hits": 43 }, { "id": 12065, "url": "https://svs.gsfc.nasa.gov/12065/", "result_type": "Produced Video", "release_date": "2015-11-18T10:00:00-05:00", "title": "Lesley Ott: Carbon and Climate Soundbite", "description": "Lesley Ott, research meteorologist in the Global Modeling and Assimilation Center at NASA's Goddard Space Flight Center, discusses how NASA is working to understand the global carbon cycle. Dr. Ott made these points on a media telecon in advance of the United Nations COP-21 climate meeting in Paris, 2015.For complete transcript, click here.Music credit: Piano Dreams by Jon Wygens || Lesley_Ott_Poster-no_text.jpg (1280x720) [219.6 KB] || Lesley_Ott_Poster-no_text_searchweb.png (320x180) [82.4 KB] || Lesley_Ott_Poster-no_text_thm.png (80x40) [17.1 KB] || Lesley_Ott_MASTER_prores.mov (1280x720) [596.5 MB] || Lesley_Ott_MASTER_youtube_hq.mov (1280x720) [137.3 MB] || Lesley_Ott_MASTER_appletv.m4v (1280x720) [20.8 MB] || Lesley_Ott_Carbon_Climate.mp4 (1280x720) [41.2 MB] || Lesley_Ott_MASTER.mpeg (1280x720) [140.0 MB] || Lesley_Ott_MASTER.webm (960x540) [16.7 MB] || Lesley_Ott_MASTER_appletv_subtitles.m4v (1280x720) [20.9 MB] || 12065_Lesley_Ott-captions.en_US.srt [953 bytes] || 12065_Lesley_Ott-captions.en_US.vtt [963 bytes] || Lesley_Ott_MASTER_ipod_sm.mp4 (320x240) [7.2 MB] || ", "hits": 20 }, { "id": 12044, "url": "https://svs.gsfc.nasa.gov/12044/", "result_type": "Produced Video", "release_date": "2015-11-12T11:00:00-05:00", "title": "Carbon and Climate Briefing - November 12, 2015", "description": "Carbon_and_Climate_HD.jpg (1280x720) [722.5 KB] || Carbon_and_Climate_HD_searchweb.png (320x180) [100.9 KB] || Carbon_and_Climate_HD_thm.png (80x40) [7.8 KB] || ", "hits": 47 }, { "id": 40269, "url": "https://svs.gsfc.nasa.gov/gallery/carbon-gallery/", "result_type": "Gallery", "release_date": "2015-11-10T00:00:00-05:00", "title": "Carbon and Climate", "description": "As carbon dioxide levels in Earth's atmosphere have increased in recent decades, the planet's land and ocean have continued to absorb about half of manmade emissions. NASA’s Earth science program works to improve our understanding of how carbon absorption and emission processes work in nature. It also seeks to track how these processes might change in a warming world with increasing levels of carbon dioxide and methane emissions from human activities.\nThe volume of carbon dioxide pumped into the atmosphere by human activities is the dominant force driving ongoing and future climate change. While NASA isn’t involved in policies around emissions levels, the agency’s scientists are targeting what can be called the \"other half\" of this carbon and climate equation – what will happen with the 50 percent of carbon dioxide emissions that are currently absorbed by the ocean, forests and other land ecosystems?\n\nThe twenty-first Conference of Parties (COP-21) to the United Nations Framework Convention on Climate Change will take place in Paris, France, November 30 to December 11, 2015. Each year, the COP meets for two weeks to discuss the state of Earth’s climate and how best to deal with future climate change. Hosted by the U.S. Department of State, the U.S. Center at COP-21 is a major public outreach initiative to inform attendees about key climate initiatives and scientific research taking place in the U.S. As has been the standard for several years, NASA scientists will be present to show examples of our ongoing research.", "hits": 204 }, { "id": 40246, "url": "https://svs.gsfc.nasa.gov/gallery/hyperwall-planets/", "result_type": "Gallery", "release_date": "2015-07-24T00:00:00-04:00", "title": "Hyperwall Planets", "description": "Hyperwall-ready visualizations featuring planets, moon, and small bodies\nReturn to Main Hyperwall Gallery.", "hits": 131 }, { "id": 11899, "url": "https://svs.gsfc.nasa.gov/11899/", "result_type": "Produced Video", "release_date": "2015-07-21T13:00:00-04:00", "title": "Scientists Link Earlier Melting Of Snow To Dark Aerosols", "description": "Tiny particles suspended in the air, known as aerosols, can darken snow and ice causing it to absorb more of the sun’s energy. But until recently, scientists rarely considered the effect of all three major types of light-absorbing aerosols together in climate models.In a new study, NASA scientists used a climate model to examine the impact of this snow-darkening phenomenon on Northern Hemisphere snowpacks, including how it affects snow amount and heating on the ground in spring.The study looked at three types of light-absorbing aerosols – dust, black carbon and organic carbon. Black carbon and organic carbon are produced from the burning of fossil fuels, like coal and oil, as well as biofuels and biomass, such as forests.With their snow darkening effect added to NASA’s GEOS-5 climate model, scientists analyzed results from 2002 to 2011, and compared them to model runs done without the aerosols on snow. They found that the aerosols indeed played a role in absorbing more of the sun’s energy. Over broad places in the Northern Hemisphere, the darkened snow caused some surface temperatures to be up to 10 degrees Fahrenheit warmer than it would be if the snow were pristine. As a result, warmer, snow-darkened areas had less snow in spring than they would have had under pristine snow conditions.According to the study, dust’s snow darkening effect significantly contributed to surface warming in Central Asia and the western Himalayas. Black carbon’s snow darkening effect had a larger impact primarily in Europe, the eastern Himalayas and East Asia. It had a smaller impact in North America. Organic carbon’s snow darkening effect was relatively lower but present in regions such as southeastern Siberia, northeastern East Asia and western Canada.“As we add more of these aerosols to the mix, we are potentially increasing our overall impact on Earth’s climate,” said research scientist Teppei Yasunari at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.Research: Impact of snow darkening via dust, black carbon, and organic carbon on boreal spring climate in the Earth systemJournal: Geophysical Research: Atmospheres, June 15, 2015.Link to paper: http://onlinelibrary.wiley.com/doi/10.1002/2014JD022977/fullHere is the YouTube video. || ", "hits": 62 }, { "id": 11898, "url": "https://svs.gsfc.nasa.gov/11898/", "result_type": "Produced Video", "release_date": "2015-06-12T12:30:00-04:00", "title": "Hubble Detects \"Sunscreen\" Layer on Distant Planet", "description": "ANIMATION Using NASA’s Hubble Telescope, scientists detected a stratosphere on the planet WASP-33b. A stratosphere occurs when molecules in the atmosphere absorb ultraviolet and visible light from the star. This absorption warms the stratosphere and acts as a kind of sunscreen layer for the planet below.Watch this video on YouTube. || CoolHotAll3av8_print.jpg (1024x576) [49.2 KB] || CoolHotAll3av8_searchweb.png (320x180) [48.2 KB] || CoolHotAll3av8_thm.png (80x40) [4.6 KB] || CoolHotAll3av8.mp4 (1920x1080) [46.7 MB] || CoolHotAll3av8sm.mp4 (1280x720) [16.4 MB] || CoolHotAll3av8sm.webm (1280x720) [2.2 MB] || ", "hits": 61 }, { "id": 11683, "url": "https://svs.gsfc.nasa.gov/11683/", "result_type": "Produced Video", "release_date": "2014-11-18T11:00:00-05:00", "title": "Simulating Carbon", "description": "Carbon dioxide is the key driver of global warming, however, despite its significance, much remains unknown about the pathways it takes from emission source to the atmosphere or carbon reservoirs such as oceans and forests. Using a NASA supercomputer model called GEOS-5, scientists created a visualization that simulates how the greenhouse gas travels through Earth’s atmosphere over the course of a year. The model run produced nearly four petabytes (million billion bytes) of data and required 75 days of dedicated computation to complete. In addition to providing a striking look at the movements of the invisible gas as it is transported by winds across the globe, the visualization illustrates differences in carbon dioxide levels in the Northern and Southern Hemispheres and distinct swings in global carbon dioxide concentrations as the growth cycle of plants and trees changes with the seasons. Watch the video for a tour of the visualization. || ", "hits": 38 }, { "id": 11583, "url": "https://svs.gsfc.nasa.gov/11583/", "result_type": "Produced Video", "release_date": "2014-07-01T12:00:00-04:00", "title": "NASA On Air: NASA Launches Satellite To Monitor Global Carbon Dioxide (7/1/2014)", "description": "LEAD: Where in the world is carbon dioxide? Where in the world does our carbon dioxide from fossil fuels go?1. NASA’s first carbon dioxide satellite launched today (7/1/2014), will measure which forests and plants soak up the most carbon dioxide from the air.2. The greater the absorption, the brighter the invisible fluorescence from growing plants.3. The U.S. corn belt is the most efficient CO2 absorber in the world!4. The Amazon rainforest is another carbon dioxide sponge.TAG: Knowing where our carbon dioxide goes will help crop forecasters, as well as climate scientists. Approximately one quarter of our carbon dioxide emissions are absorbed by forests and vegetation. || WC_OCO-1920-MASTER_iPad_960x540.0_print.jpg (1280x720) [59.9 KB] || WC_OCO-1920-MASTER_iPad_1920x0180_searchweb.png (320x180) [42.0 KB] || WC_OCO-1920-MASTER_iPad_1920x0180_web.png (320x180) [42.0 KB] || WC_OCO-1920-MASTER_iPad_1920x0180_thm.png (80x40) [3.8 KB] || WC_OCO-1920-MASTER_1920x1080.mov (1920x1080) [604.3 MB] || WC_OCO-1920-MASTER_1280x720.mov (1280x720) [727.0 MB] || WC_OCO-1920-MASTER_NBC_Today.mov (1920x1080) [188.9 MB] || WC_OCO-1920-MASTER_WEA_CEN.wmv (1280x720) [16.8 MB] || OCO_.avi (1280x720) [18.6 MB] || WC_OCO-1920-MASTER_baron.mp4 (1920x1080) [24.3 MB] || WC_OCO-1920-MASTER_prores.mov (1920x1080) [534.9 MB] || WC_OCO-1920-MASTER_iPad_960x540.m4v (960x540) [61.8 MB] || WC_OCO-1920-MASTER_iPad_1280x720.m4v (1280x720) [95.7 MB] || WC_OCO-1920-MASTER_iPad_1920x0180.m4v (1920x1080) [188.9 MB] || WC_OCO-1920-MASTER_iPad_960x540.webmhd.webm (960x540) [4.9 MB] || ", "hits": 25 }, { "id": 30515, "url": "https://svs.gsfc.nasa.gov/30515/", "result_type": "Hyperwall Visual", "release_date": "2014-06-30T13:00:00-04:00", "title": "Simulated Atmospheric Carbon Concentrations", "description": "Carbon exists in many forms—e.g., carbon dioxide (CO2), carbon monoxide (CO)—and continually cycles through Earth’s atmosphere, ocean, and terrestrial ecosystems. This visualization, created using data from the 7-km GEOS-5 Nature Run model, shows average column concentrations of atmospheric CO2 (colored shades) and CO (white shades underneath) from January 1, 2006 to December 31, 2006.CO2 variations are largely controlled by fossil fuel emissions and seasonal fluxes of carbon between the atmosphere and land biosphere. For example, dark red and pink shades represent regions where CO2 concentrations are enhanced by carbon sources, mainly from human activities. During Northern Hemisphere spring and summer months, plants absorb a substantial amount of CO2 through photosynthesis, thus removing CO2 from the atmosphere. Atmospheric CO, a pollutant harmful to human health, is produced mainly from fossil fuel combustion and biomass burning. Here, high concentrations of CO (white) are mainly from fire activity in Africa, South America, and Australia. Scientists use model output data such as these to help answer important questions about Earth’s climate and to help design future satellite missions.These model simulations use fossil fuel emissions estimates provided by the Emissions Database for Global Atmospheric Research (EDGAR). NASA’s Quick Fire Emissions Dataset (QFED) estimates fire emissions using MODIS fire radiative power observations. Additional, observationally constrained estimates of CO2 flux between the atmosphere and land and ocean carbon reservoirs were produced as part of NASA’s Carbon Monitoring System Flux Pilot Project (http://carbon.nasa.gov/cgi-bin/cms/inv_pgp.pl?pgid=581). Land biosphere fluxes come from the Carnegie-Ames-Stanford Approach Global Fire Emissions Database (CASA-GFED) model which incorporates MODIS vegetation classification and AVHRR Normalized Difference Vegetation Index (NDVI) data. Ocean fluxes are produced by the NASA Ocean Biogeochemical Model (NOBM) which incorporates MODIS chlorophyll observations. || ", "hits": 104 }, { "id": 4128, "url": "https://svs.gsfc.nasa.gov/4128/", "result_type": "Visualization", "release_date": "2013-12-24T00:00:00-05:00", "title": "Solar Dynamics Observatory - Argo view - Slices of SDO", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections. This visualization is a variation of the original Solar Dynamics Observatory - Argo view. In this case, the different wavelength filters are presented in three sets around the Sun at full 4Kx4K resolution. This enables monitoring of changes in time over all wavelengths at any location around the limb of the Sun. The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.if we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.in far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "hits": 96 }, { "id": 4117, "url": "https://svs.gsfc.nasa.gov/4117/", "result_type": "Visualization", "release_date": "2013-12-17T10:00:00-05:00", "title": "Solar Dynamics Observatory - Argo view", "description": "Argos (or Argus Panoptes) was the 100-eyed giant in Greek mythology (wikipedia).While the Solar Dynamics Observatory (SDO) has significantly less than 100 eyes, (see \"SDO Jewelbox: The Many Eyes of SDO\"), seeing connections in the solar atmosphere through the many filters of SDO presents a number of interesting challenges. This visualization experiment illustrates a mechanism for highlighting these connections.The wavelengths presented are: 617.3nm optical light from SDO/HMI. From SDO/AIA we have 170nm (pink), then 160nm (green), 33.5nm (blue), 30.4nm (orange), 21.1nm (violet), 19.3nm (bronze), 17.1nm (gold), 13.1nm (aqua) and 9.4nm (green).We've locked the camera to rotate the view of the Sun so each wedge-shaped wavelength filter passes over a region of the Sun. As the features pass from one wavelength to the next, we can see dramatic differences in solar structures that appear in different wavelengths.Filaments extending off the limb of the Sun which are bright in 30.4 nanometers, appear dark in many other wavelengths.Sunspots which appear dark in optical wavelengths, are festooned with glowing ribbons in ultraviolet wavelengths.Small flares, invisible in optical wavelengths, are bright ribbons in ultraviolet wavelengths.If we compare the visible light limb of the Sun with the 170 nanometer filter on the left, with the visible light limb and the 9.4 nanometer filter on the right, we see that the 'edge' is at different heights. This effect is due to the different amounts of absorption, and emission, of the solar atmosphere in ultraviolet light.In far ultraviolet light, the photosphere is dark since the black-body spectrum at a temperature of 5700 Kelvin emits very little light in this wavelength. || ", "hits": 119 }, { "id": 11428, "url": "https://svs.gsfc.nasa.gov/11428/", "result_type": "Produced Video", "release_date": "2013-12-03T12:00:00-05:00", "title": "Alien Atmospheres", "description": "Since the early 1990's, astronomers have known that extrasolar planets, or \"exoplanets,\" orbit stars light-years beyond our own solar system. Although most exoplanets are too distant to be directly imaged, detailed studies have been made of their size, composition, and even atmospheric makeup - but how? By observing periodic variations in the parent star's brightness and color, astronomers can indirectly determine an exoplanet's distance from its star, its size, and its mass. But to truly understand an exoplanet astronomers must study its atmosphere, and they do so by splitting apart the parent star's light during a planetary transit. || ", "hits": 295 }, { "id": 30380, "url": "https://svs.gsfc.nasa.gov/30380/", "result_type": "Hyperwall Visual", "release_date": "2013-10-24T12:00:00-04:00", "title": "Monthly Net Primary Productivity", "description": "Plants play an important role in the movements of carbon dioxide throughout Earth's environment. Living plants both take in carbon dioxide from the air and put out carbon dioxide to the air. Called net primary productivity, these maps show where and how much carbon dioxide is taken in by vegetation during photosynthesis minus how much carbon dioxide is released when plants respire on a monthly basis, from February 2000 to the present. Created using data from the Moderate Resolutions Imaging Spectroradiometer (MODIS) instrument onboard NASA’s Terra satellite, the colors on these maps indicate how fast carbon was taken in for every square meter of land. Values range from -1.0 grams of carbon per square meter per day (tan) to 6.5 grams per square meter per day (dark green). A negative value means decomposition or respiration overpowered carbon absorption; more carbon was released to the atmosphere than the plants took in. Maps such as these allow scientists to routinely monitor plants' role in the global carbon cycle. || ", "hits": 190 }, { "id": 30385, "url": "https://svs.gsfc.nasa.gov/30385/", "result_type": "Hyperwall Visual", "release_date": "2013-10-24T12:00:00-04:00", "title": "Monthly Cloud Optical Thickness (Terra/MODIS)", "description": "To better understand the role of clouds in the Earth's climate system, scientists need two important measurements: cloud optical thickness and cloud particle size. A cloud's optical thickness is a measure of attenuation of the light passing through the atmosphere due to the scattering and absorption by cloud droplets. Clouds do not absorb visible wavelengths of sunlight; rather, clouds scatter and reflect most visible light. The higher a cloud's optical thickness, the more sunlight the cloud is scattering and reflecting. These maps show monthly cloud optical thickness from January 2005 to the present, produced using data from the Moderate Resolution Imaging Spectroradiometer (MODIS) instrument onboard NASA’s Terra satellite. Dark blue shades indicate areas where there are low cloud-optical-thickness values, while white shades indicate high values (i.e., greater attenuation caused by the scattering and absorption from cloud droplets). || ", "hits": 167 }, { "id": 30398, "url": "https://svs.gsfc.nasa.gov/30398/", "result_type": "Hyperwall Visual", "release_date": "2013-10-24T12:00:00-04:00", "title": "Monthly Cloud Optical Thickness (Aqua/MODIS)", "description": "To better understand the role of clouds in the Earth's climate system, scientists need two important measurements: cloud optical thickness and cloud particle size. A cloud's optical thickness is a measure of attenuation of the light passing through the atmosphere due to the scattering and absorption by cloud droplets. Clouds do not absorb visible wavelengths of sunlight; rather, clouds scatter and reflect most visible light. The higher a cloud's optical thickness, the more sunlight the cloud is scattering and reflecting. These maps show monthly cloud optical thickness from July 2002 to the present, produced using data from the Moderate Resolution Imaging Spectroradiometer (MODIS) instrument onboard NASA’s Aqua satellite. Dark blue shades indicate areas where there are low cloud-optical-thickness values, while white shades indicate high values (i.e., greater attenuation caused by the scattering and absorption from cloud droplets). || ", "hits": 64 }, { "id": 30356, "url": "https://svs.gsfc.nasa.gov/30356/", "result_type": "Hyperwall Visual", "release_date": "2013-10-22T12:00:00-04:00", "title": "Uranus in True and False Color", "description": "These two pictures of Uranus — one in true color (left) and the other in false color — were compiled from images returned Jan. 17, 1986, by the narrow-angle camera of Voyager 2. The spacecraft was 9.1 million kilometers (5.7 million miles) from the planet, several days from closest approach. The picture at left has been processed to show Uranus as human eyes would see it from the vantage point of the spacecraft. The picture is a composite of images taken through blue, green and orange filters. The darker shadings at the upper right of the disk correspond to the day-night boundary on the planet. Beyond this boundary lies the hidden northern hemisphere of Uranus, which currently remains in total darkness as the planet rotates. The blue-green color results from the absorption of red light by methane gas in Uranus' deep, cold and remarkably clear atmosphere. The picture at right uses false color and extreme contrast enhancement to bring out subtle details in the polar region of Uranus. Images obtained through ultraviolet, violet and orange filters were respectively converted to the same blue, green and red colors used to produce the picture at left. The very slight contrasts visible in true color are greatly exaggerated here. In this false-color picture, Uranus reveals a dark polar hood surrounded by a series of progressively lighter concentric bands. One possible explanation is that a brownish haze or smog, concentrated over the pole, is arranged into bands by zonal motions of the upper atmosphere. The bright orange and yellow strip at the lower edge of the planet's limb is an artifact of the image enhancement. In fact, the limb is dark and uniform in color around the planet. The Voyager project is managed for NASA by the Jet Propulsion Laboratory. || ", "hits": 194 }, { "id": 30138, "url": "https://svs.gsfc.nasa.gov/30138/", "result_type": "Hyperwall Visual", "release_date": "2013-10-17T12:00:00-04:00", "title": "SOFIA view Jupiter in Infrared", "description": "Infrared image of Jupiter from SOFIA's First Light flight composed of individual images at wavelengths of 5.4 (blue), 24 (green) and 37 microns (red) made by Cornell University's FORCAST camera. Ground-based infrared observations are impossible at 5.4 and 37 microns and normally very difficult at 24 microns even from high mountaintop observatories such as Mauna Kea due to absorption by water and other molecules in Earth's atmosphere. The white stripe in the infrared image is a region of relatively transparent clouds through which the warm interior of Jupiter can be seen. A recent visual-wavelength picture of approximately the same side of Jupiter is shown for comparison. (Images are oriented with Jupiter's south pole at the top.) || ", "hits": 77 }, { "id": 20199, "url": "https://svs.gsfc.nasa.gov/20199/", "result_type": "Animation", "release_date": "2013-05-20T00:00:00-04:00", "title": "The California Laboratory for Atmospheric Remote Sensing", "description": "The Megacities Carbon Project is developing and testing methods for monitoring the greenhouse gas emissions of cities, the largest human contributors to climate change. One of the sites in the Megacities monitoring network for Los Angeles is the California Laboratory for Atmospheric Remote Sensing (CLARS) located on Mt Wilson. From an altitude of nearly 6000 ft, CLARS makes frequent scans during daylight hours across the LA basin. In this animation, the CLARS telescope mirror points sequentially to different pre-programmed points to sample sunlight scattering off the Earth's surface. The CLARS spectrometer splits the light from each reflection point into a spectrum (like colors in a rainbow) to reveal the unique \"fingerprints\" of carbon dioxide, methane and other gases in the atmosphere. The lines in the spectrum are due to absorption from the various gases - analysis of which is used to reveal the concentration of a given gas in a column of air for a given location. CLARS serves as a prototype for a future geostationary satellite instrument that may someday serve as a \"carbon weather satellite\" - providing frequent wall-to-wall mapping of greenhouse gases across entire cities and broader regions.CLARS was developed by JPL with support from the NASA Earth Science Technology Office. CLARS operations are funded jointly by NASA and NIST. || ", "hits": 18 }, { "id": 30007, "url": "https://svs.gsfc.nasa.gov/30007/", "result_type": "Hyperwall Visual", "release_date": "2013-03-14T00:00:00-04:00", "title": "MODIS Cloud Optical Thickness", "description": "NASA’s Global Modeling and Assimilation Office (GMAO) works to maximize the impact of NASA’s satellite observations in weather and climate analysis and prediction through integrated Earth system modeling and data assimilation.This visualization compares cloud optical thickness from a GMAO simulation using the Goddard Earth Observing System Model, Version 5 (GEOS-5) [top] to observations from the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard Aqua and Terra [bottom], August 17-26, 2009. A cloud's optical thickness is a measure of attenuation of the light passing through the atmosphere due to the scattering and absorption by cloud droplets. Clouds do not absorb visible wavelengths of sunlight; rather, clouds scatter and reflect most visible light. Here, light blue shades indicate areas where there are low cloud-optical-thickness values, while red and orange shades indicate high values (i.e., greater attenuation caused by the scattering and absorption from cloud droplets). The higher a cloud's optical thickness, the more sunlight the cloud is scattering and reflecting. || ", "hits": 64 }, { "id": 4043, "url": "https://svs.gsfc.nasa.gov/4043/", "result_type": "Visualization", "release_date": "2013-03-06T11:00:00-05:00", "title": "LRO Peers into Permanent Shadows", "description": "The Moon's permanently shadowed regions, or PSRs, are places on the Moon that haven't seen the Sun in millions, or even billions, of years. The Earth's tilted axis allows sunlight to fall everywhere on its surface, even at the poles, for at least part of the year. But the Moon's tilt relative to the Sun is only 1.6°, not enough to get sunlight into some deep craters near the lunar north and south poles. PSRs are therefore some of the coldest, darkest places in the solar system.Because of that, PSRs are expected to be excellent traps for volatiles, chemicals that would normally vaporize and escape into space, and this includes water. Lunar Reconnaissance Orbiter (LRO) includes several instruments designed to peer into the PSR darkness and measure temperature, reflectivity, and neutron absorption, all of which are clues to what chemicals might be hiding there. This animation shows where the PSRs are and in what ways LRO can see inside them. || ", "hits": 511 }, { "id": 11117, "url": "https://svs.gsfc.nasa.gov/11117/", "result_type": "Produced Video", "release_date": "2012-11-01T14:00:00-04:00", "title": "NASA's Fermi Explores the Early Universe", "description": "Astronomers using data from NASA's Fermi Gamma-ray Space Telescope have made the most accurate measurement of starlight in the universe and used it to establish the total amount of light from all of the stars that have ever shone, accomplishing a primary mission goal.Gamma rays are the most energetic form of light. Since Fermi's launch in 2008, its Large Area Telescope (LAT) observes the entire sky in high-energy gamma rays every three hours, creating the most detailed map of the universe ever known at these energies. The total sum of starlight in the cosmos is known to astronomers as the extragalactic background light (EBL). To gamma rays, the EBL functions as a kind of cosmic fog. Ajello and his team investigated the EBL by studying gamma rays from 150 blazars, or galaxies powered by black holes, that were strongly detected at energies greater than 3 billion electron volts (GeV), or more than a billion times the energy of visible light. As matter falls toward a galaxy's supermassive black hole, some of it is accelerated outward at almost the speed of light in jets pointed in opposite directions. When one of the jets happens to be aimed in the direction of Earth, the galaxy appears especially bright and is classified as a blazar.Gamma rays produced in blazar jets travel across billions of light-years to Earth. During their journey, the gamma rays pass through an increasing fog of visible and ultraviolet light emitted by stars that formed throughout the history of the universe. Occasionally, a gamma ray collides with starlight and transforms into a pair of particles — an electron and its antimatter counterpart, a positron. Once this occurs, the gamma ray light is lost. In effect, the process dampens the gamma-ray signal in much the same way as fog dims a distant lighthouse. From studies of nearby blazars, scientists have determined how many gamma rays should be emitted at different energies. More distant blazars show fewer gamma rays at higher energies — especially above 25 GeV — thanks to absorption by the cosmic fog. The farthest blazars are missing most of their higher-energy gamma rays.The researchers then determined the average gamma-ray attenuation across three distance ranges between 9.6 billion years ago and today. From this measurement, the scientists were able to estimate the fog's thickness. To account for the observations, the average stellar density in the cosmos is about 1.4 stars per 100 billion cubic light-years. To put this in another way, the average distance between stars in the universe is about 4,150 light-years.See the media briefing page here. || ", "hits": 115 }, { "id": 11012, "url": "https://svs.gsfc.nasa.gov/11012/", "result_type": "Produced Video", "release_date": "2012-07-17T00:00:00-04:00", "title": "A Sky For All Seasons", "description": "Globally, carbon dioxide levels remain on a steady, long-term rise. However, concentrations of the heat-trapping gas are distributed unevenly around the world and change with the seasons. NASA's ability to track these changes by satellite, first achieved in 2008, provides a new way to study the interaction between carbon dioxide and the vegetation that absorbs it from the atmosphere. As plant life begins to draw the greenhouse gas from the air each spring, carbon dioxide levels plunge. When plants go dormant in winter, levels start to rise. The visualization illustrates this relationship by layering NASA satellite data of carbon dioxide levels over a global map of vegetation growth from 2003 to 2006. Notice the cyclical changes in carbon dioxide levels in the Northern Hemisphere compared to the Southern Hemisphere. The significantly larger population and landmass north of the equator makes for both increased human-caused emissions and carbon dioxide absorption. || ", "hits": 33 }, { "id": 3842, "url": "https://svs.gsfc.nasa.gov/3842/", "result_type": "Visualization", "release_date": "2011-06-24T00:00:00-04:00", "title": "Carbon Catch And Release", "description": "Through tiny, microscopic pores called stomata, plants absorb one hundred billion tons of carbon from the air each year and convert about half of that into organic matter—leaves, roots, tree branches, grass. As we continue to increase the level of carbon dioxide in the atmosphere, knowing exactly how much carbon Earth's plants absorb from the air—Gross Primary Productivity (GPP)—will become only more important. NASA has closely measured this since 2000, and that volume of absorption is seen in the first visualization below as waves of green. The northern hemisphere all the way up to the Arctic Circle swells with life each summer, before much of the vegetation wilts and exhales its carbon in fall and winter. Meanwhile, forests such as the Amazon, a robust green throughout, show off their amazing productivity despite seasonal changes. || ", "hits": 54 }, { "id": 10630, "url": "https://svs.gsfc.nasa.gov/10630/", "result_type": "Produced Video", "release_date": "2010-08-19T14:00:00-04:00", "title": "Plant Productivity in a Warming World", "description": "The past decade is the warmest on record since instrumental measurements began in the 1880s. Previous research suggested that in the '80s and '90s, warmer global temperatures and higher levels of precipitation — factors associated with climate change — were generally good for plant productivity. An updated analysis published this week in Science indicates that as temperatures have continued to rise, the benefits to plants are now overwhelmed by longer and more frequent droughts. High-resolution data from the Moderate Resolution Imaging Spectroradiometer, or MODIS, indicate a net decrease in NPP from 2000-2009, as compared to the previous two decades. || ", "hits": 19 }, { "id": 3638, "url": "https://svs.gsfc.nasa.gov/3638/", "result_type": "Visualization", "release_date": "2009-10-09T00:00:00-04:00", "title": "Correlation Between Tropospheric Carbon Dioxide Concentration and Seasonal Variation of the Biosphere", "description": "This animation shows the correspondence between the drawdown of tropospheric carbon dioxide in the earth's atmosphere, and the seasonal variation of the biosphere of the earth. The pattern of white squares indicates regions where the concentration of tropospheric CO2 is higher than the trend, while regions devoid of the squares are areas where the CO2 concentrations are lower than the trend. The trend was calculated by a least-squares line fit to a moving 8-day global average of CO2 concentration provided by the AIRS instrument on the Aqua satellite, and increases over the course of the animation (Sept. 2002-Sept. 2006) from 374 ppm to 383 ppm. The biosphere data is provided by the SeaWiFS instrument aboard the SeaStar satellite.During spring and summer months, the consumption of CO2 through plant respiration increases, reducing the concentration of CO2 (the white squares) over the more productive areas. In the animation, this is seen as a tendency for the CO2 concentration to drop below the trend over areas of deeper green. The cycle is especially apparent in the Northern Hemisphere. || ", "hits": 79 }, { "id": 10494, "url": "https://svs.gsfc.nasa.gov/10494/", "result_type": "Produced Video", "release_date": "2009-10-09T00:00:00-04:00", "title": "The Carbon Cycle", "description": "Carbon is the basic building block of life, and these unique atoms are found everywhere on Earth. Carbon makes up Earth's plants and animals, and is also stored in the ocean, the atmosphere, and the crust of the planet. A carbon atom could spend millions of years moving through Earth in a complex cycle. This conceptual animation provides an illustration of the various parts of the Carbon cycle. Purple arrows indicate the uptake of Carbon; yellow arrows indicate the release of Carbon. On land, plants remove carbon from the atmosphere through photosynthesis. Animals eat plants and either breath out the carbon, or it moves up the food chain. When plants and animals die and decay, they transfer carbon back to the soil. Moving offshore, the ocean takes up carbon through physical and biological processes. At the ocean's surface, carbon dioxide from the atmosphere dissolves into the water. Tiny marine plants called phytoplankton use this carbon dioxide for photosynthesis. Phytoplankton are the base of the marine food web. After animals eat the plants, they breathe out the carbon or pass it up the food chain. Sometimes phytoplankton die, decompose, and are recycled in the surface waters. Phytoplankton can also sink to the bottom of the ocean, where they become buried in marine sediment. Over long time scales, this process has made the ocean floor the largest reservoir of carbon on the planet. In a process called upwelling, currents bring cold water containing carbon up to the surface. As the water warms, the carbon is then be released as a gas back into the atmosphere, continuing the carbon cycle. Carbon is found in the atmosphere as Carbon dioxide, which is a greenhouse gas. Greenhouse gases act like a blanket, and trap heat in the atmosphere. In the past two centuries, humans have increased atmospheric carbon dioxide by more than 30%, by burning fossil-fuels and cutting down forests. || ", "hits": 314 }, { "id": 10389, "url": "https://svs.gsfc.nasa.gov/10389/", "result_type": "Produced Video", "release_date": "2009-02-19T00:00:00-05:00", "title": "Aerosols Absorb; Aerosols Reflect", "description": "Some aerosol particles primarily reflect solar radiation and cool the atmosphere, and others can also absorb radiation and warm the surrounding air. When aerosols heat the atmosphere, they create an unstable environment where clouds can't thrive. The suppression of clouds leads to further warming of the atmosphere by solar radiation. Aerosols are a complex but critical piece of the climate puzzle, and researchers are still working to understand the role of these curious particles. || ", "hits": 169 }, { "id": 10395, "url": "https://svs.gsfc.nasa.gov/10395/", "result_type": "Produced Video", "release_date": "2009-02-19T00:00:00-05:00", "title": "Earth's Energy Budget Animations: Global View and Budget Breakout", "description": "Total solar irradiance (TSI) is the dominant driver of the Earth's climate. The global temperature of the Earth is almost completely determined by the balance between the intensity of the incident solar radiation and the response of the Earth's atmosphere via absorption, reflection, and re-radiation. Roughly 30 percent of the TSI that strikes the Earth is reflected back into space by clouds, atmospheric aerosols, snow, ice, desert sand, rooftops, and even ocean surf. The remaining 70 percent of the TSI is absorbed by the land, ocean, and atmosphere. In addition, different layers of the Earth's atmosphere absorb different wavelengths of light. Changes in either the TSI or in the composition of the atmosphere can cause climate change. Two conceptual science animations provide two different perspectives that both illustrate Earth's energy budget. || ", "hits": 88 }, { "id": 10201, "url": "https://svs.gsfc.nasa.gov/10201/", "result_type": "Produced Video", "release_date": "2008-04-14T00:00:00-04:00", "title": "LRO Instrument Integrations", "description": "The LRO payload, comprised of six instruments and one technology demonstration, will provide key data sets to enable a human return to the moon. Though built at a variety of partner institutions, all of LRO's instruments were integrated onto the spacecraft at NASA's Goddard Space Flight Center. || ", "hits": 81 }, { "id": 20092, "url": "https://svs.gsfc.nasa.gov/20092/", "result_type": "Animation", "release_date": "2006-10-05T00:00:00-04:00", "title": "Earth's Energy Budget Breakout", "description": "Reigning on Earth's Climate - Only about 70% of the solar energy that reaches Earth is absorbed, while the other 30% is reflected back into space by atmosphere and aerosols, ocean/land and clouds. A closer view reveals a delicate balance between absorption and reflection as well as a release of energy by rocks, air and sea warming and emitting increasing amounts of thermal radiation (heat) in the form of long-wave infrared light. This radiation allows Earth to lose heat at the same rate it gains from the Sun. Evidence is in the land/ocean interaction, the absorption of energy by clouds, water vapor and the greenhouse gas ozone, as well as the 20-24% absorbed and emitted back by clouds. || ", "hits": 85 }, { "id": 20093, "url": "https://svs.gsfc.nasa.gov/20093/", "result_type": "Animation", "release_date": "2006-10-05T00:00:00-04:00", "title": "Earth's Energy Budget Global View", "description": "Reigning on Earth's Climate - Only about 70% of the solar energy that reaches Earth is absorbed, while the other 30% is reflected back into space by atmosphere and aerosols, ocean/land and clouds. A closer view reveals a delicate balance between absorption and reflection as well as a release of energy by rocks, air and sea warming and emitting increasing amounts of thermal radiation (heat) in the form of long-wave infrared light. This radiation allows Earth to lose heat at the same rate it gains from the Sun. Evidence is in the land/ocean interaction, the absorption of energy by clouds, water vapor and the greenhouse gas ozone, as well as the 20-24% absorbed and emitted back by clouds. || ", "hits": 25 }, { "id": 20094, "url": "https://svs.gsfc.nasa.gov/20094/", "result_type": "Animation", "release_date": "2006-10-05T00:00:00-04:00", "title": "Earth's Energy Budget: Land", "description": "Reigning on Earth's Climate - Only about 70% of the solar energy that reaches Earth is absorbed, while the other 30% is reflected back into space by atmosphere and aerosols, ocean/land and clouds. A closer view reveals a delicate balance between absorption and reflection as well as a release of energy by rocks, air and sea warming and emitting increasing amounts of thermal radiation (heat) in the form of long-wave infrared light. This radiation allows Earth to lose heat at the same rate it gains from the Sun. Evidence is in the land/ocean interaction, the absorption of energy by clouds, water vapor and the greenhouse gas ozone, as well as the 20-24% absorbed and emitted back by clouds. || ", "hits": 30 }, { "id": 20095, "url": "https://svs.gsfc.nasa.gov/20095/", "result_type": "Animation", "release_date": "2006-10-05T00:00:00-04:00", "title": "Earth's Energy Budget: Water Vapor", "description": "Reigning on Earth's Climate - Only about 70% of the solar energy that reaches Earth is absorbed, while the other 30% is reflected back into space by atmosphere and aerosols, ocean/land and clouds. A closer view reveals a delicate balance between absorption and reflection as well as a release of energy by rocks, air and sea warming and emitting increasing amounts of thermal radiation (heat) in the form of long-wave infrared light. This radiation allows Earth to lose heat at the same rate it gains from the Sun. Evidence is in the land/ocean interaction, the absorption of energy by clouds, water vapor and the greenhouse gas ozone, as well as the 20-24% absorbed and emitted back by clouds. || ", "hits": 438 }, { "id": 3175, "url": "https://svs.gsfc.nasa.gov/3175/", "result_type": "Visualization", "release_date": "2005-06-21T00:00:00-04:00", "title": "Outgoing Shortwave Flux Compared to Clouds (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the reflected solar radiation measured by CERES during 29 orbits on June 20 and 21 of 2003 over infrared cloud images for the same period. Reflected solar radiation is shortwave radiation, and the most intense reflection comes from clouds. || ", "hits": 24 }, { "id": 3176, "url": "https://svs.gsfc.nasa.gov/3176/", "result_type": "Visualization", "release_date": "2005-06-21T00:00:00-04:00", "title": "Outgoing Longwave Flux Compared to Clouds (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the outgoing thermal radiation measured by CERES during 29 orbits on June 20 and 21 of 2003 over global infrared cloud images. Thermal radiation is longwave radiation and depends on the temperature of the earth, with the most intense radiation coming from the warmest regions and the least from cold clouds in the atmosphere. Although cold clouds and the cold Antarctic night regions can be seen in this data, the Earth radiates pretty uniformly in the longwave bands because the atmosphere distributes the heat of the sun to the whole planet. || ", "hits": 31 }, { "id": 3177, "url": "https://svs.gsfc.nasa.gov/3177/", "result_type": "Visualization", "release_date": "2005-06-21T00:00:00-04:00", "title": "Net Radiation Flux Compared to Clouds (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the net radiation flux within view of CERES during 29 orbits on June 20 and 21 of 2003. The net flux is the incoming solar flux minus the outgoing reflected (shortwave) and thermal (longwave) radiation. If the flux in a region is positive, the Earth is being warmed by the sun in that region, while cooling regions have a negative flux. It is clear from the animation that the most intensive heating occurs in ocean regions with few clouds, while the second most intense are cloud-free regions over vegetated land areas. Deserts, cloudy regions, and ice caps all reflect enough solar radiation to reduce the amount of heating. Regions of night are, of course, cooling regions because there is no incoming flux at all. || ", "hits": 62 }, { "id": 3178, "url": "https://svs.gsfc.nasa.gov/3178/", "result_type": "Visualization", "release_date": "2005-06-21T00:00:00-04:00", "title": "Incoming Solar Flux Compared to Clouds (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure. Note that the infrared cloud image shown under the solar data shows high infrared as dark (land) and low infrared as light (clouds). || ", "hits": 35 }, { "id": 3179, "url": "https://svs.gsfc.nasa.gov/3179/", "result_type": "Visualization", "release_date": "2005-06-21T00:00:00-04:00", "title": "Scene Identification Compared to Clouds (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time. || ", "hits": 10 }, { "id": 3089, "url": "https://svs.gsfc.nasa.gov/3089/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Clear-sky Albedo (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average clear-sky albedo from July, 2002 through June, 2004 as measured by the CERES instrument. This is the fraction of the incoming solar radiation that is reflected back into space by regions of the Earth on cloud-free days. The regions of highest albedo are regions of snow and ice, followed by desert regions. Oceans have the lowest albedo, and reflect very little of the incoming solar radiation. It is not possible to measure the albedo during the winter months at the poles, since there is no incoming solar radiation during these times. || ", "hits": 47 }, { "id": 3090, "url": "https://svs.gsfc.nasa.gov/3090/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Total-sky Albedo (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average albedo from July, 2002 through June, 2004 as measured by the CERES instrument. This is the fraction of the incoming solar radiation that is reflected back into space by regions of the Earth. The regions of highest albedo are regions of snow and ice, followed by desert regions and regions where there is significant cloud cover during the year. Oceans have the lowest albedo. It is not possible to measure the albedo during the winter months at the poles, since there is no incoming solar radiation during these times. || ", "hits": 52 }, { "id": 3091, "url": "https://svs.gsfc.nasa.gov/3091/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Clear-sky Outgoing Longwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average clear-sky outgoing longwave radiation from July, 2002 through June, 2004 as measured by the CERES instrument. This is the thermal radiation given off by the warm Earth when the sky is cloud free. The Earth's rotation and the movement of warm air from the equator to the poles make the Earth roughly uniformin temperature. The most visible features are the cold poles in winter and the significant regions of snow coverage in the northern hemisphere, also in winter. || ", "hits": 18 }, { "id": 3092, "url": "https://svs.gsfc.nasa.gov/3092/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Total-sky Outgoing Longwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average outgoing longwave radiation from July, 2002 through June, 2004 as measured by the CERES instrument. This is the thermal radiation given off by the warm Earth. The Earth's rotation and the movement of warm air from the equator to the poles make the Earth roughly uniform in temperature. The most visible features are the cold poles in winter and the cold clouds along the equator which trap the outgoing thermal radiation. || ", "hits": 19 }, { "id": 3093, "url": "https://svs.gsfc.nasa.gov/3093/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Clear-sky Net Radiant Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly clear-sky average net radiant flux from July, 2002 through June, 2004 as measured by the CERES instrument. This is the incoming radiation minus the outgoing reflected or thermal energy given off by areas of the Earth when the sky is cloud-free. Regions in red and yellow have a net incoming flux and are being heated. Regions in blue have a net outgoing flux and are being cooled. Regions in black are in rough equilibrium. Summertime oceans are heated the most, while high latitude winter regions are cooled the most, probably because of the longer winter nights. Note that the Earth's ice sheets are almost always regions of cooling. On average, the heating and cooling amounts must balance, or the Earth will change temperature and the climate will change. || ", "hits": 43 }, { "id": 3094, "url": "https://svs.gsfc.nasa.gov/3094/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Total-sky Net Radiant Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average net radiant flux from July, 2002 through June, 2004 as measured by the CERES instrument. This is the incoming radiation minus the outgoing reflected or thermal energy given off by areas of the Earth. Regions in red and yellow have a net incoming flux and are being heated. Regions in blue have a net outgoing flux and are being cooled. Regions in black are in rough equilibrium. Cloud-free summertime oceans are heated the most, while high latitude winter regions are cooled the most, probably because of the longer winter nights. Note that regions that reflect a lot of sunlight, such as the polar ice sheets and the Sahara desert are almost always in equilibrium or are cooling regions. || ", "hits": 33 }, { "id": 3095, "url": "https://svs.gsfc.nasa.gov/3095/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Total-sky Incoming Solar Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average incoming solar radiation from July, 2002 through June, 2004 as measured by the CERES instrument. This average data set is constant in longitude because of the Earth's rotation, but clearly shows the seasonal cycle as the sun heats the Northern Hemisphere more in summer than in winter. Note that the polar regions are abnormally bright in the local summer and dark in the local winter because whole day is either light or dark in those seasons. || ", "hits": 29 }, { "id": 3096, "url": "https://svs.gsfc.nasa.gov/3096/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Clear-sky Outgoing Shortwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average clear-sky outgoing shortwave radiation from July, 2002 through June, 2004 as measured by the CERES instrument. This is the sunlight that is directly reflected back into space by ice, desert, and other physical areas on the Earth when the sky is cloud-free. The ice sheets can be clearly seen to reflect the most sunlight, with desert areas next. Oceans absorb the most sunlight, more than the vegetated land areas such as the tropical rain forest and temperate forests and plains. || ", "hits": 21 }, { "id": 3097, "url": "https://svs.gsfc.nasa.gov/3097/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Average Total-sky Outgoing Shortwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The average amount of reflection and absorption is critical to the climate, because the absorbed energy heats up the Earth until it is radiated away as thermal radiation. This animation shows the monthly average outgoing shortwave radiation from July, 2002 through June, 2004 as measured by the CERES instrument. This is the sunlight that is directly reflected back into space by clouds, ice, desert, and other physical areas on the Earth. Although clouds are very reflective, they come and going during the month, so more reflection is seen on average from ice sheets, which change very little during a monthly period. Note that the cloud-free parts of the ocean are relatively dark, indicating that oceans absorb more sunlight than they reflect. || ", "hits": 13 }, { "id": 3104, "url": "https://svs.gsfc.nasa.gov/3104/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Instantaneous Scene Identification (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to th e climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time. || ", "hits": 16 }, { "id": 3105, "url": "https://svs.gsfc.nasa.gov/3105/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Instantaneous Incoming Solar Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure. || ", "hits": 92 }, { "id": 3106, "url": "https://svs.gsfc.nasa.gov/3106/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Instantaneous Net Radiation Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the net radiation flux within view of CERES during 29 orbits on June 20 and 21 of 2003. The net flux is the incoming solar flux minus the outgoing reflected (shortwave) and thermal (longwave) radiation. If the flux in a region is positive, the Earth is being warmed by the sun in that region, while cooling regions have a negative flux. It is clear from the animation that the most intensive heating occurs in ocean regions with few clouds, while the second most intense are cloud-free regions over vegetated land areas. Deserts, cloudy regions, and ice caps all reflect enough solar radiation to reduce the amount of heating. Regions of night are, of course, cooling regions because there is no incoming flux at all. || ", "hits": 33 }, { "id": 3107, "url": "https://svs.gsfc.nasa.gov/3107/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Instantaneous Outgoing Longwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the outgoing thermal radiation measured by CERES during 29 orbits on June 20 and 21 of 2003. Thermal radiation is longwave radiation and depends on the temperature of the earth, with the most intense radiation coming from the warmest regions and the least from cold clouds in the atmosphere. Although cold clouds and the cold Antarctic night regions can be seen in this data, the Earth radiates pretty uniformly in the longwave bands because the atmosphere distributes the heat of the sun to the whole planet. || ", "hits": 8 }, { "id": 3108, "url": "https://svs.gsfc.nasa.gov/3108/", "result_type": "Visualization", "release_date": "2005-02-01T12:00:00-05:00", "title": "Instantaneous Outgoing Shortwave Flux (WMS)", "description": "The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the reflected solar radiation measured by CERES during 29 orbits on June 20 and 21 of 2003. Reflected solar radiation is shortwave radiation, and the most intense reflection comes from clouds, followed by ice. Land reflects only a small amount of radiation, but ocean reflects the least, which is the reason that the sun heats the oceans so effectively. Of course, there is no reflected solar radiation in regions of night. || ", "hits": 13 }, { "id": 20006, "url": "https://svs.gsfc.nasa.gov/20006/", "result_type": "Animation", "release_date": "2003-11-05T12:00:00-05:00", "title": "Carbon Cycle", "description": "The Carbon Cycle - The carbon cycle on land, acted out here show a tree taking in carbon dioxide from the atmosphere, and combined with water and nutrients from the soil, growing. In the fall and winter, parts of the growth die off and release some carbon back into the system. At some point, the tree is no longer able to take in carbon and begins to die. When that happens, all the carbon absorbed in its body is released back into the cycle as it decomposes. Fire can accelerate this, sending plumes of carbon-laden aerosols into the atmosphere, as well as leaving carbon-rich ash deposits on the ground for further decomposition and recycling. || ", "hits": 25 }, { "id": 20007, "url": "https://svs.gsfc.nasa.gov/20007/", "result_type": "Animation", "release_date": "2003-11-05T12:00:00-05:00", "title": "Carbon Cycle", "description": "Carbon And The Ocean — The Slow Cycle - The oceans are vast, and their processes as complex as their waters are deep.Phytoplankton absorbs carbon dioxide from the atmosphere and nutrient rich waters and grows in wide colonies called blooms. These blooms are highly dependent on surrounding environmental conditions.As phytoplankton grows, it forms the foundation for the food chain, thus passing carbon up to higher life forms. But just as on land, links in the ocean's chain of life also break, and stored carbon settles out of the top layers of water. A portion of it gets swept back to the surface as upwellings, only to begin again, but a major portion sinks to the bottom, becoming what oceanographers call 'marine snow.' This decomposing biological matter literally precipitates through the water and builds up on the ocean bottom, essentially sequestered from the rest of the Earth for geologically long periods of time. || ", "hits": 167 }, { "id": 40116, "url": "https://svs.gsfc.nasa.gov/gallery/jwst/", "result_type": "Gallery", "release_date": "2000-01-01T00:00:00-05:00", "title": "James Webb Space Telescope", "description": "The James Webb Space Telescope (sometimes called JWST) is a large, infrared-optimized space telescope. The observatory launched into space on an Ariane 5 rocket from the Guiana Space Centre in Kourou, French Guiana on December 25, 2021. After launch, the observatory was successfully unfolded and is being readied for science. \n\nWebb will find the first galaxies that formed in the early Universe, connecting the Big Bang to our own Milky Way Galaxy. Webb will peer through dusty clouds to see stars forming planetary systems, connecting the Milky Way to our own Solar System. Webb's instruments are designed to work primarily in the infrared range of the electromagnetic spectrum, with some capability in the visible range.\n\nWebb has a large primary mirror, 6.5 meters (21.3 feet) in diameter and a sunshield the size of a tennis court. Both the mirror and sunshade are too large to fit onto the Ariane 5 rocket fully open, so both were folded which meant they needed to be unfolded in space. \n\nWebb is currently in its operational orbit about 1.5 million km (1 million miles) from the Earth at a location known as Lagrange Point 2 (L2).\n\nThe James Webb Space Telescope was named after the NASA Administrator who crafted the Apollo program, and who was a staunch supporter of space science.", "hits": 864 }, { "id": 812, "url": "https://svs.gsfc.nasa.gov/812/", "result_type": "Visualization", "release_date": "1999-04-09T12:00:00-04:00", "title": "HALOE Looking at the Sun", "description": "The Halogen Occultation Experiment, HALOE, was designed to carefully monitor hydrogen fluoride and hydrogen chloride, byproducts of CFC destruction in the stratosphere. HALOE operates by observing the absorption of infrared radiation by these molecules against the rising and setting sun. || ", "hits": 35 }, { "id": 830, "url": "https://svs.gsfc.nasa.gov/830/", "result_type": "Visualization", "release_date": "1999-04-09T12:00:00-04:00", "title": "HALOE Measurements of HCl in the Stratosphere (1992 - 1998)", "description": "HALOE was designed to carefully monitor hydrogen fluoride and hydrogen chloride, byproducts of CFC destruction in the stratosphere. HALOE operates by observing the absorption of infrared radiation by these molecules against the rising and setting sun. When UARS was first launched, measurements by HALOE showed that CFC byproducts were still increasing in the stratosphere. But the newest HALOE measurements now show that CFC by-products are no longer increasing. UARS has shown that the stratosphere is starting to respond to the international ban on CFC manufacture. || ", "hits": 43 }, { "id": 60, "url": "https://svs.gsfc.nasa.gov/60/", "result_type": "Visualization", "release_date": "1994-05-20T12:00:00-04:00", "title": "Nonlinear Studies of Coronal Heating by the Resonant Absorption of Alfven Waves", "description": "A series of animations showing various quantities from a coronal heating simulation || a000060.00005_web.png (720x480) [280.0 KB] || a000060_thm.png (80x40) [3.6 KB] || a000060_pre.jpg (320x238) [5.4 KB] || a000060_pre_searchweb.jpg (320x180) [25.3 KB] || a000060.webmhd.webm (960x540) [48.4 MB] || a000060.dv (720x480) [653.3 MB] || a000060.mp4 (640x480) [37.5 MB] || a000060.mpg (352x240) [29.3 MB] || ", "hits": 68 }, { "id": 1603, "url": "https://svs.gsfc.nasa.gov/1603/", "result_type": "Visualization", "release_date": "1990-07-10T12:00:00-04:00", "title": "Support Animations/Stills for SOLVE", "description": "The polar vortex || Vortex.jpg (640x480) [47.7 KB] || newVORTEX_pre.jpg (320x240) [9.5 KB] || Vortex_thm.png (80x40) [5.5 KB] || newVORTEX_pre_searchweb.jpg (180x320) [66.0 KB] || newVORTEX.webmhd.webm (960x540) [1.6 MB] || Vortex.tif (640x480) [253.9 KB] || newVORTEX.mov (320x240) [4.2 MB] || ", "hits": 17 } ] }