{ "count": 17, "next": null, "previous": null, "results": [ { "id": 31294, "url": "https://svs.gsfc.nasa.gov/31294/", "result_type": "Hyperwall Visual", "release_date": "2024-06-17T00:00:00-04:00", "title": "PACE Observes Namesake Plankton, Aerosols, Clouds and Ocean Ecosystem", "description": "Beautiful images from PACE show phytoplankton being swirled about by ocean currents of the coast off North America and in the Black Sea. || ", "hits": 121 }, { "id": 14204, "url": "https://svs.gsfc.nasa.gov/14204/", "result_type": "Produced Video", "release_date": "2022-08-31T09:00:00-04:00", "title": "Mars Patchy Proton Aurora", "description": "NASA’s MAVEN (Mars Atmosphere and Volatile Evolution) mission and the United Arab Emirates’ Emirates Mars Mission (EMM) have released joint observations of dynamic proton aurora events at Mars. Remote auroral observations by EMM paired with in-situ plasma observations made by MAVEN open new avenues for understanding the Martian atmosphere. This collaboration was made possible by recent data-sharing between the two missions and highlights the value of multi-point observations in space.Learn more about this discovery by MAVEN and EMM. || ", "hits": 100 }, { "id": 31027, "url": "https://svs.gsfc.nasa.gov/31027/", "result_type": "Hyperwall Visual", "release_date": "2019-03-25T10:00:00-04:00", "title": "Triangulum Galaxy Mosaic", "description": "Full Hubble mosaic image of the Triangulum galaxy (M33), composed of 54 Hubble fields of view stitched together. The borders of individual Hubble images trace the jagged edge of the mosaic, which spans 19,400 light-years across. || STSCI-H-p1901a-f-32073x41147_print.jpg (1024x1313) [262.9 KB] || STSCI-H-p1901a-q-8019x10287.png (8019x10287) [134.5 MB] || STSCI-H-p1901a-h-16307x20574.png (16037x20574) [542.5 MB] || STSCI-H-p1901a-f-32073x41147_searchweb.png (320x180) [73.3 KB] || STSCI-H-p1901a-f-32073x41147_thm.png (80x40) [5.8 KB] || STSCI-H-p1901a-f-32073x41147.tif.dzi (32073x41147) [181 bytes] || STSCI-H-p1901a-f-32073x41147.tif_files (1x1) [4.0 KB] || STSCI-H-p1901a-f-32073x41147.tif (32073x41147) [1.7 GB] || ", "hits": 123 }, { "id": 30994, "url": "https://svs.gsfc.nasa.gov/30994/", "result_type": "Hyperwall Visual", "release_date": "2018-10-15T10:00:00-04:00", "title": "Messier 82: Cigar Galaxy in Multiple Wavelengths", "description": "Massive burst of star formation in the core or M82 burst becomes clearer in infrared. || STScI-H-M82_1x-1920x1080.00001_print.jpg (1024x576) [79.3 KB] || STScI-H-M82_1x-1920x1080.00001_searchweb.png (320x180) [66.4 KB] || STScI-H-M82_1x-1920x1080.00001_thm.png (80x40) [4.5 KB] || STScI-H-M82_1x-1280x720.mp4 (1280x720) [5.0 MB] || STScI-H-M82_1x-1920x1080.mp4 (1920x1080) [11.8 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-M82_1x-1920x1080.webm (1920x1080) [5.2 MB] || STSCI-H-M82_1x-3840x2160.mp4 (3840x2160) [12.8 MB] || STSCI-H-M82_1x-H265-3840x2160.mp4 (3840x2160) [6.0 MB] || STScI-H-M82_1x-640x360.mp4 (640x360) [1.6 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 110 }, { "id": 30969, "url": "https://svs.gsfc.nasa.gov/30969/", "result_type": "Hyperwall Visual", "release_date": "2018-06-18T10:00:00-04:00", "title": "M101 (Pinwheel Galaxy)", "description": "This animation shows the Messier 101 (Pinwheel) Galaxy, with simulated rotation, in visible, then infrared, then X-ray, and finally all three combined. || STScI-H-M101_1x-1920x1080.00001_print.jpg (1024x576) [150.4 KB] || STScI-H-M101_1x-1920x1080.00001_searchweb.png (320x180) [99.4 KB] || STScI-H-M101_1x-1920x1080.00001_thm.png (80x40) [6.3 KB] || STScI-H-M101_1x-1280x720.mp4 (1280x720) [18.1 MB] || STScI-H-M101_1x-1920x1080.mp4 (1920x1080) [50.6 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-M101_1x-1920x1080.webm (1920x1080) [5.6 MB] || STScI-H-M101_1x-640x360.mp4 (640x360) [7.8 MB] || STScI-H-M101_1x-3840x2160.mp4 (3840x2160) [32.3 MB] || STScI-H-M101_1x-H265-3840x2160.mp4 (3840x2160) [11.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 231 }, { "id": 30960, "url": "https://svs.gsfc.nasa.gov/30960/", "result_type": "Hyperwall Visual", "release_date": "2018-06-04T10:00:00-04:00", "title": "Eagle Nebula: M16 Wide", "description": "This series of images shows the environment around the Pillars of Creation, the Eagle Nebula, Messier 16. The images reveal the nebula in optical, X-ray, mid-infrared, and far-infrared light. || STScI-H-M16wide_1x-1920x1080.00001_print.jpg (1024x576) [163.7 KB] || STScI-H-M16wide_1x-1920x1080.00001_searchweb.png (320x180) [108.4 KB] || STScI-H-M16wide_1x-1920x1080.00001_thm.png (80x40) [6.9 KB] || STScI-H-M16wide_1x-1280x720.mp4 (1280x720) [8.5 MB] || STScI-H-M16wide_1x-1920x1080.mp4 (1920x1080) [17.9 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-M16wide_1x-1920x1080.webm (1920x1080) [5.2 MB] || STScI-H-M16wide_1x-640x360.mp4 (640x360) [2.9 MB] || STScI-H-M16wide_1x-3840x2160.mp4 (3840x2160) [17.1 MB] || STScI-H-M16wide_1x-H265-3840x2160.mp4 (3840x2160) [7.6 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 175 }, { "id": 30959, "url": "https://svs.gsfc.nasa.gov/30959/", "result_type": "Hyperwall Visual", "release_date": "2018-05-28T10:00:00-04:00", "title": "The Orion Nebula: Visible and Infrared Views", "description": "This animation showcases the Orion Nebula, first in infrared light (Spitzer), then in visible light (Hubble), and finally a blend of the two images in a multi-color mosaic. || STScI-H-Orion_1x-1920x1080.00001_print.jpg (1024x576) [71.8 KB] || STScI-H-Orion_1x-1920x1080.00001_searchweb.png (320x180) [54.4 KB] || STScI-H-Orion_1x-1920x1080.00001_thm.png (80x40) [4.1 KB] || STScI-H-Orion_1x-1280x720.mp4 (1280x720) [4.5 MB] || STScI-H-Orion_1x-1920x1080.mp4 (1920x1080) [8.5 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-Orion_1x-1280x720.webm (1280x720) [4.1 MB] || STScI-H-Orion_1x-640x360.mp4 (640x360) [2.1 MB] || STScI-H-Orion_1x-3840x2160.mp4 (3840x2160) [9.7 MB] || STScI-H-Orion_1x-H265_3840x2160.mp4 (3840x2160) [3.7 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 489 }, { "id": 30952, "url": "https://svs.gsfc.nasa.gov/30952/", "result_type": "Hyperwall Visual", "release_date": "2018-05-21T10:00:00-04:00", "title": "The Whirlpool Galaxy: Visible and X-ray Views", "description": "This animation contrasts the visible-light (Hubble Space Telescope) and X-ray (Chandra X-ray Observatory) images of Messier 51, the majestic Whirlpool galaxy. || STScI-H-M51-Whirlpool_1x-1920x1080.00001_print.jpg (1024x576) [193.0 KB] || STScI-H-M51-Whirlpool_1x-1920x1080.00001_searchweb.png (320x180) [105.6 KB] || STScI-H-M51-Whirlpool_1x-1920x1080.00001_thm.png (80x40) [6.7 KB] || STScI-H-M51-Whirlpool_1x-1280x720.mp4 (1280x720) [6.2 MB] || STScI-H-M51-Whirlpool_1x-1920x1080.mp4 (1920x1080) [14.5 MB] || STScI-H-M51-Whirlpool_1x-1920x1080.webm (1920x1080) [3.0 MB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || STScI-H-M51-Whirlpool_1x-640x360.mp4 (640x360) [1.8 MB] || STScI-H-M51-Whirlpool_1x-3840x2160.mp4 (3840x2160) [12.4 MB] || STScI-H-M51-Whirlpool_1x-H265-3840x2160.mp4 (3840x2160) [6.2 MB] || 3840x2160_16x9_30p (3840x2160) [0 Item(s)] || ", "hits": 218 }, { "id": 11796, "url": "https://svs.gsfc.nasa.gov/11796/", "result_type": "Produced Video", "release_date": "2015-03-05T14:00:00-05:00", "title": "Mars’ Ancient Ocean", "description": "NASA planetary scientists Geronimo Villanueva and Michael Mumma discuss their findings regarding the ancient ocean of Mars.Watch this video on the NASAexplorer YouTube channel.For complete transcript, click here. || Mars_Ocean_still_print.jpg (1024x576) [113.5 KB] || Mars_Ocean_still.png (1920x1080) [3.0 MB] || Mars_Ocean_still_web.jpg (320x180) [16.0 KB] || Mars_Ocean_still_searchweb.png (320x180) [86.4 KB] || Mars_Ocean_still_thm.png (80x40) [8.2 KB] || G2015-011_MarsOcean_MASTER_appletv.webm (960x540) [30.9 MB] || G2015-011_MarsOcean_MASTER_ipod_lg.m4v (640x360) [46.0 MB] || G2015-011_MarsOcean_MASTER_ipod_sm.mp4 (320x240) [24.8 MB] || G2015-011_MarsOcean_MASTER.en_US.srt [4.4 KB] || G2015-011_MarsOcean_MASTER.en_US.vtt [4.4 KB] || G2015-011_MarsOcean_MASTER_prores.mov (1280x720) [4.0 GB] || G2015-011_MarsOcean_MASTER_youtube_hq.mov (1280x720) [187.8 MB] || G2015-011_MarsOcean_MASTER_appletv.m4v (960x540) [116.1 MB] || G2015-011_MarsOcean_MASTER_1280x720.wmv (1280x720) [136.4 MB] || G2015-011_MarsOcean_MASTER_appletv_subtitles.m4v (960x540) [116.0 MB] || G2015-011_MarsOcean_MASTER_nasaportal.mov (640x360) [112.8 MB] || ", "hits": 522 }, { "id": 11339, "url": "https://svs.gsfc.nasa.gov/11339/", "result_type": "Produced Video", "release_date": "2013-09-30T12:00:00-04:00", "title": "Propylene on Titan", "description": "With a thick atmosphere, clouds, a rain cycle and giant lakes, Saturn's large moon Titan is a surprisingly Earthlike place. But unlike on Earth, Titan's surface is far too cold for liquid water - instead, Titan's clouds, rain, and lakes consist of liquid hydrocarbons like methane and ethane (which exist as gases here on Earth). When these hydrocarbons evaporate and encounter ultraviolet radiation in Titan's upper atmosphere, some of the molecules are broken apart and reassembled into longer hydrocarbons like ethylene and propane.NASA's Voyager 1 spacecraft first revealed the presence of several species of atmospheric hydrocarbons when it flew by Titan in 1980, but one molecule was curiously missing - propylene, the main ingredient in plastic number 5. Now, thanks to NASA's Cassini spacecraft, scientists have detected propylene on Titan for the first time, solving a long-standing mystery about the solar system's most Earthlike moon. || ", "hits": 143 }, { "id": 11295, "url": "https://svs.gsfc.nasa.gov/11295/", "result_type": "Produced Video", "release_date": "2013-06-13T11:00:00-04:00", "title": "MAVEN Imaging Ultraviolet Spectrograph", "description": "The philosophy of NASA's Mars Program has been \"Follow the water,\" but \"Where did the atmosphere go?\" is still a lingering question. Although fluvial features such as dry riverbeds are visible on Mars, the atmosphere today is too thin to support liquid water, implying that Mars once had a thicker atmosphere that was lost to space. NASA's Mars Atmosphere and Volatile EvolutioN Mission, or MAVEN, will test this hypothesis. As part of its remote sensing instrument package, MAVEN's Imaging Ultraviolet Spectrograph (IUVS) will look at isotopic hydrogen ratios in the upper atmosphere of Mars, helping scientists to determine just how much water once flowed across the Red Planet. || ", "hits": 59 }, { "id": 11292, "url": "https://svs.gsfc.nasa.gov/11292/", "result_type": "Produced Video", "release_date": "2013-06-03T11:00:00-04:00", "title": "Water on the Moon", "description": "Since the 1960’s, scientists have suspected that frozen water could survive in cold, dark craters at the Moon’s poles. While previous lunar missions have detected hints of water on the Moon, new data from the Lunar Reconnaissance Orbiter (LRO) pinpoints areas near the south pole where water is likely to exist. The key to this discovery is hydrogen, the main ingredient in water: LRO uses its Lunar Exploration Neutron Detector, or LEND, to measure how much hydrogen is trapped within the lunar soil. By combining years of LEND data, scientists see mounting evidence of hydrogen-rich areas near the Moon’s south pole, strongly suggesting the presence of frozen water. || ", "hits": 180 }, { "id": 3690, "url": "https://svs.gsfc.nasa.gov/3690/", "result_type": "Visualization", "release_date": "2010-03-28T00:00:00-04:00", "title": "Lunar Reconnaissance Orbiter Releases Data to the Planetary Data System", "description": "On March 15, 2010, Lunar Reconnaissance Orbiter (LRO) released its first installment of scientific data to NASA's public archive for planetary data, the Planetary Data System (PDS). This animation highlights several of the datasets made available through the PDS by the LOLA, LEND, and Diviner instruments on LRO. || ", "hits": 97 }, { "id": 3480, "url": "https://svs.gsfc.nasa.gov/3480/", "result_type": "Visualization", "release_date": "2008-09-30T00:00:00-04:00", "title": "Lunar Prospector Hydrogen Concentration - South Pole", "description": "In 1998 NASA's Lunar Prospector mission used the presence of hydrogen as a sign of potential ice deposits. As you can see in this video, Prospector data showed significantly more hydrogen at the south pole of the moon (areas colored blue). Lunar Reconnaissance Orbiter will build on this data and narrow down the regions that may contain water ice deposits. || ", "hits": 105 }, { "id": 2510, "url": "https://svs.gsfc.nasa.gov/2510/", "result_type": "Visualization", "release_date": "2002-08-28T12:00:00-04:00", "title": "Mars Odyssey Science Cover Image", "description": "This still was created to for the cover of the journal Science (5 July 2002 issue). It shows epithermal neutron data represented by the colors overlayed on Mars topography. The blue colors represent high concentrations of hydrogen, indicating the strong possibility that water ice exists in those regions.The vertical exaggeration is 5x normal and the shading exaggeration is 50x normal. || ", "hits": 7 }, { "id": 40, "url": "https://svs.gsfc.nasa.gov/40/", "result_type": "Visualization", "release_date": "1994-02-12T12:00:00-05:00", "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Hydrogen Mass Fraction", "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ", "hits": 93 }, { "id": 41, "url": "https://svs.gsfc.nasa.gov/41/", "result_type": "Visualization", "release_date": "1994-02-12T12:00:00-05:00", "title": "Rayleigh-Taylor Instabilities in Supernovae Explosions: Partial Density of Hydrogen", "description": "The following calculation shows the development and evolution of Rayleigh-Taylor instabilities which develop behind the supernova blast wave on a time scale of a few hours. The initial model was chosen to provide a good representation for the progenitor star for Supernova 1987A. The calculation was performed using the Piecewise-Parabolic Method for hydrodynamics on a two-dimensional spherical grid with rotational symmetry about the vertical axis and equatorial symmetry about the horizontal axis.The grid contained 800 zones in the radial direction and 400 zones in the angular diraction and was allowed to expand homologously with the explosion to maintain as high a resolution as possible in the unstable layer during the evolution. The following sequences show the evolution of the density distribution as well as the distribution of hydrogen, helium, and oxygen within the ejecta to illustrate the amount of mixing caused by the instability. Each sequence shows the evolution in two reference frames.In the first frame, the size of the plot expands with time as the grid expands. For the second reference frame, the size of the plot is kept fixed with the time so that more detail can be seen in the unstable layer. || ", "hits": 43 } ] }