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    "results": [
        {
            "id": 14957,
            "url": "https://svs.gsfc.nasa.gov/14957/",
            "result_type": "Produced Video",
            "release_date": "2026-01-27T10:00:00-05:00",
            "title": "IMAP Arrives at L1",
            "description": "NASA’s IMAP (Interstellar Mapping and Acceleration Probe) reached its destination at Lagrange point 1, or L1, approximately 1 million miles from Earth toward the Sun on Jan. 10, 2026.The mission’s operations team sent commands to the spacecraft on the morning of Jan. 9 to begin trajectory maneuvers to enter orbit at L1. Early on the morning of Jan. 10, the team confirmed the spacecraft had successfully entered its final L1 orbit, where it will stay for the duration of its mission.From L1, IMAP will explore and map the very boundaries of our heliosphere — the protective bubble created by the solar wind that encapsulates our entire solar system — and study how the heliosphere interacts with the local galactic neighborhood beyond.Learn more about the milestone: https://science.nasa.gov/blogs/imap/2026/01/12/nasas-imap-mission-reaches-its-destination/ || ",
            "hits": 368
        },
        {
            "id": 14895,
            "url": "https://svs.gsfc.nasa.gov/14895/",
            "result_type": "Produced Video",
            "release_date": "2025-09-17T10:00:00-04:00",
            "title": "Mapping the Boundaries of Our Home in Space with NASA’s IMAP Mission",
            "description": "NASA’s new Interstellar Mapping and Acceleration Probe, or IMAP, will explore and map the very boundaries of our heliosphere — a huge bubble created by the Sun's wind that encapsulates our solar system — and study how that boundary interacts with the local galactic neighborhood beyond.As a modern-day celestial cartographer, IMAP will chart the vast range of particles in interplanetary space, helping to investigate two of the most important overarching issues in heliophysics — the energization of charged particles from the Sun, and the interaction of the solar wind with interstellar space. Additionally, IMAP will support near real-time observations of the solar wind and energetic particles, which can produce hazardous conditions in the space environment near Earth. IMAP is launching no earlier than Sept. 23, 2025, aboard a SpaceX Falcon 9 rocket from Launch Complex 39A at NASA’s Kennedy Space Center in Florida.Learn more about IMAP science: https://science.nasa.gov/missions/nasas-imap-mission-to-study-boundaries-of-our-home-in-space/Find out more about the IMAP mission: https://science.nasa.gov/mission/imap/ || ",
            "hits": 181
        },
        {
            "id": 14897,
            "url": "https://svs.gsfc.nasa.gov/14897/",
            "result_type": "Produced Video",
            "release_date": "2025-09-16T10:00:00-04:00",
            "title": "Our Interstellar Medium",
            "description": "Our Milky Way galaxy is home to more than 100 billion stars that are often separated by trillions of miles. The spaces in between, called the interstellar medium, aren't empty –– they're sprinkled with gas and dust that are both the seeds of new stars and the leftover crumbs from stars long dead. Studying the interstellar medium with observatories like NASA’s upcoming Nancy Grace Roman Space Telescope will reveal new insight into the galactic dust recycling system.Music Credit: Building Heroes by Enrico Cacace [BMI], Universal Production MusicCredit: NASA's Goddard Space Flight CenterWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || Our_Interstellar_Medium_Thumbnail.jpg (1280x720) [658.8 KB] || Our_Interstellar_Medium_Thumbnail_searchweb.png (320x180) [105.7 KB] || Our_Interstellar_Medium_Thumbnail_thm.png (80x40) [7.3 KB] || Our_Interstellar_Medium.en_US.srt [1.1 KB] || Our_Interstellar_Medium.en_US.vtt [1.0 KB] || 14897_-_Our_Interstellar_Medium.mp4 (3840x2160) [651.7 MB] || 14897_-_Our_Interstellar_Medium_-_NO_TEXT.mov (3840x2160) [3.7 GB] || ",
            "hits": 300
        },
        {
            "id": 20363,
            "url": "https://svs.gsfc.nasa.gov/20363/",
            "result_type": "Animation",
            "release_date": "2022-03-09T18:00:00-05:00",
            "title": "Animation: Heliosphere",
            "description": "The sun sends out a constant flow of charged particles called the solar wind, which ultimately travels past all the planets to some three times the distance to Pluto before being impeded by the interstellar medium. This forms a giant bubble around the sun and its planets, known as the heliosphere. NASA studies the heliosphere to better understand the fundamental physics of the space surrounding us - which, in turn, provides information regarding space throughout the rest of the universe, as well as regarding what makes planets habitable.The solar wind is a gas of charged particles known as plasma, a state of matter governed by its own set physical laws just as the more common solids, liquids, and gases are. As the solar wind sweeps out into space, it creates a space environment filled with radiation as well as magnetic fields that trail all the way back to the sun. This space environment is augmented by interstellar cosmic rays and occasional concentrated clouds of solar material that burst off the sun, known as coronal mass ejections.This complex environment surrounds the planets and ultimately has a crucial effect on the formation, evolution, and destiny of planetary systems. For one thing, our heliosphere acts as a giant shield, protecting the planets from galactic cosmic radiation. Earth is additionally shielded by its own magnetic field, the magnetosphere, which protects us not only from solar and cosmic particle radiation but also from erosion of the atmosphere by the solar wind. Planets without a shielding magnetic field, such as Mars and Venus, are exposed to such processes and have evolved differently.NASA's studies of the heliosphere include research into: how the solar wind behaves near Earth; what causes and sustains magnetic and electric fields around other planets; how does the heliosphere interact with the interstellar medium; what do the boundaries of the heliosphere look like; what is the origin and evolution of the solar wind and the interstellar cosmic rays; and what contributes to the habitability of exoplanets.The field is, therefore, intensely cross-disciplinary. Heliospheric research often works hand in hand with planetary scientists, astrophysicists, astrobiologists, and space weather researchers.NASA heliophysics missions contributing to heliospheric research are: the Advanced Composition Explorer; NOAA's Deep Space Climate Observatory, the Interstellar Boundary Explorer, the Solar Terrestrial Relations Observatory; Voyager, and Wind. || ",
            "hits": 455
        },
        {
            "id": 13642,
            "url": "https://svs.gsfc.nasa.gov/13642/",
            "result_type": "Produced Video",
            "release_date": "2020-06-11T10:00:00-04:00",
            "title": "11 Years Charting The Edge of The Solar System",
            "description": "Watch this video on the NASA Goddard YouTube channel.Music credits: “End of Days - Joe Mason Remix” by Connor Shambrook [BMI], Cyrus Reynolds [BMI], Flynn Hase Spence [ASCAP], Joseph Scott Mason [APRA]; “Brainstorming” by Laurent Dury [SACEM]; “Flight of the Leaf Remix” by Julie Gruss [GEMA], Laurent Dury [SAXEM]; “Ticks and Thoughts” by Laurent Dury [SACEM]; “Intimate Journey” by Laurent Vernerey [SACEM], Nicolas de Ferran [SACEM] from Universal Production MusicComplete transcript available. || 13642_IBEX11years_YouTube.00214_print.jpg (1024x576) [239.3 KB] || 13642_IBEX11years_YouTube.00214_searchweb.png (320x180) [98.0 KB] || 13642_IBEX11years_YouTube.00214_thm.png (80x40) [6.7 KB] || 13642_IBEX11years_Prores-2.mov (1920x1080) [4.2 GB] || 13642_IBEX11years_YouTube.mp4 (1920x1080) [489.0 MB] || 13642_IBEX11years_Facebook.mp4 (1920x1080) [366.4 MB] || 13642_IBEX11years_Twitter.mp4 (1920x1080) [66.4 MB] || 13642_IBEX11years_YouTube.webm (1920x1080) [33.9 MB] || IBEX11years.en_US.srt [5.8 KB] || IBEX11years.en_US.vtt [5.8 KB] || ",
            "hits": 87
        },
        {
            "id": 12639,
            "url": "https://svs.gsfc.nasa.gov/12639/",
            "result_type": "Produced Video",
            "release_date": "2017-09-05T10:00:00-04:00",
            "title": "Where is the Edge of the Solar System?",
            "description": "Complete transcript available.Music credit: Dream Girl 3 by Yuri Sazonoff || EdgeofSolarSystem_ThumbnailOption2_print.jpg (1024x576) [252.4 KB] || EdgeofSolarSystem_ThumbnailOption2.png (3840x2160) [14.7 MB] || EdgeofSolarSystem_ThumbnailOption2_thm.png (80x40) [7.0 KB] || EdgeofSolarSystem_ThumbnailOption2_searchweb.png (320x180) [115.1 KB] || 12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_appletv.m4v (1280x720) [28.8 MB] || 12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_appletv_subtitles.m4v (1280x720) [28.8 MB] || YOUTUBE_1080_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_youtube_1080.webm (1920x1080) [7.2 MB] || TWITTER_720_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_twitter_720.mp4 (1280x720) [12.3 MB] || YOUTUBE_1080_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_youtube_1080.mp4 (1920x1080) [95.1 MB] || FACEBOOK_720_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_facebook_720.mp4 (1280x720) [70.5 MB] || YOUTUBE_720_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_youtube_720.mp4 (1280x720) [96.0 MB] || PRORES_B-ROLL_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_prores.mov (1280x720) [403.5 MB] || 12639_Edge_of_the_Solar_System.en_US.srt [810 bytes] || 12639_Edge_of_the_Solar_System.en_US.vtt [823 bytes] || YOUTUBE_4K_12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_youtube_4k.mp4 (3840x2160) [246.9 MB] || 12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_lowres.mp4 (480x272) [9.5 MB] || 12639_EdgeofSolarSystem_Final_24fps_v02_VX-718267_youtube_hq.mov (3840x2160) [1.8 GB] || 12639_EdgeofSolarSystem_Final_24fps_v02.mov (3840x2160) [3.0 GB] || 12639_EdgeofSolarSystem_Final_2997fps_v02.mov (3840x2160) [3.7 GB] || ",
            "hits": 340
        },
        {
            "id": 11821,
            "url": "https://svs.gsfc.nasa.gov/11821/",
            "result_type": "Produced Video",
            "release_date": "2015-03-25T14:00:00-04:00",
            "title": "Suzaku, Herschel Link a Black-hole 'Wind' to a Galactic Gush",
            "description": "This movie illustrates how black-hole feedback works in quasars. Dense gas and dust in the center simultaneously fuels the black hole and shrouds it from view. The black-hole wind propels large-scale outflows of cold gas and powers a shock wave that clears gas and dust from the central galaxy.Video credit: NASA's Goddard Space Flight Center || Suzaku_Quasar_Wind_STILL.png (1920x1080) [8.1 MB] || Suzaku_Quasar_Wind_STILL_print.jpg (1024x576) [41.8 KB] || Suzaku_Quasar_Wind_STILL_searchweb.png (320x180) [55.0 KB] || Suzaku_Quasar_Wind_STILL_web.png (320x180) [55.0 KB] || Suzaku_Quasar_Wind_STILL_thm.png (80x40) [7.9 KB] || 11821_Suzaku_Quasar_Wind_FINAL_appletv.webm (960x540) [3.3 MB] || 11821_Suzaku_Quasar_Wind_FINAL.mov (1920x1080) [333.5 MB] || 1920x1080_16x9_30p (1920x1080) [32.0 KB] || 11821_Suzaku_Quasar_Wind_FINAL-H264_Best_1920x1080_2997.mov (1920x1080) [295.2 MB] || 11821_Suzaku_Quasar_Wind_FINAL-H264_Good_1920x1080_2997.mov (1920x1080) [36.8 MB] || 11821_Suzaku_Quasar_Wind_FINAL-MPEG4_1920X1080_2997.mp4 (1920x1080) [13.0 MB] || 11821_Suzaku_Quasar_Wind_FINAL_1280x720.wmv (1280x720) [13.8 MB] || 11821_Suzaku_Quasar_Wind_FINAL_appletv.m4v (960x540) [13.6 MB] || 11821_Suzaku_Quasar_Wind_FINAL_ipod_lg.m4v (640x360) [5.2 MB] || 11821_Suzaku_Quasar_Wind_FINAL_ipod_sm.mp4 (320x240) [2.6 MB] || ",
            "hits": 36
        },
        {
            "id": 30571,
            "url": "https://svs.gsfc.nasa.gov/30571/",
            "result_type": "Hyperwall Visual",
            "release_date": "2015-01-15T00:00:00-05:00",
            "title": "Science with SOFIA",
            "description": "First image in presentation || sofia_montage_print.jpg (1024x575) [201.0 KB] || sofia_montage.png (4098x2304) [7.8 MB] || sofia_montage_searchweb.png (320x180) [106.7 KB] || sofia_montage_web.png (320x179) [106.7 KB] || sofia_montage_thm.png (80x40) [8.4 KB] || randolf_klein_sofia.hwshow [60 bytes] || Dr. Randolf Klein's AAS presentation from January 2015 || ",
            "hits": 25
        },
        {
            "id": 11550,
            "url": "https://svs.gsfc.nasa.gov/11550/",
            "result_type": "Produced Video",
            "release_date": "2014-07-28T13:00:00-04:00",
            "title": "NASA X-ray Instrument Confirms the 'Local Hot Bubble'",
            "description": "New findings from the NASA-funded Diffuse X-ray emission from the Local Galaxy (DXL) mission have resolved a decades-old puzzle about a fog of low-energy X-rays observed over the entire sky. Using refurbished detectors first flown on a NASA sounding rocket in the 1970s, astronomers have now confirmed the long-held suspicion that much of this glow stems from a region of million-degree interstellar plasma known as the local hot bubble, or LHB.In the 1990s, a six-month all-sky survey by the German X-ray observatory ROSAT provided improved maps of the soft X-ray diffuse background. But it also revealed that comets were an unexpected source of soft X-rays. As scientists began to understand this process, called solar wind charge exchange, they realized it could occur anywhere neutral atoms interacted with the solar wind, leading scientists to challenge the LHB interpretation.On Dec. 12, 2012, DXL launched from White Sands Missile Range in New Mexico atop a NASA Black Brant IX sounding rocket, reaching a peak altitude of 160 miles (258 km) and spending five minutes above Earth's atmosphere. The mission design allowed the instrument to observe a worst-case scenario involving charge exchange with interstellar gas.The solar system is currently passing through a small cloud of cold interstellar gas as it moves through the galaxy. The cloud’s neutral hydrogen and helium atoms stream through the planetary system at about 56,000 mph (90,000 km/h). While hydrogen atoms quickly ionize and respond to numerous forces, the helium atoms travel paths largely governed by the sun's gravity. This creates a \"helium focusing cone\" downstream from the sun that crosses Earth's orbit and is located high in the sky near midnight in early December. Better still, it forms a region with a much greater density of neutral atoms and a correspondingly enhanced charge exchange rate.The solar wind originates in the sun's corona, the hottest part of its atmosphere, so its atoms have been ionized, stripped of many of their electrons. When these particles collide with a neutral atom, one of its electrons often jumps to the solar wind ion. Once captured, the electron briefly remains in an excited state, then emits a soft X-ray and settles down at a lower energy.  To establish a baseline for the soft X-ray background, the researchers used data captured by the ROSAT mission in September 1990 in a direction looking along, rather than into, the helium focusing cone. The results indicate that only about 40 percent of the soft X-ray background originates within the solar system, which means the LHB is the dominant source. || ",
            "hits": 134
        },
        {
            "id": 30474,
            "url": "https://svs.gsfc.nasa.gov/30474/",
            "result_type": "Hyperwall Visual",
            "release_date": "2013-11-01T12:00:00-04:00",
            "title": "Voyager 1 Exits Heliosphere",
            "description": "At 122 times our distance from the sun, NASA's Voyager 1 spacecraft is the first human-made object to leave the heliosphere, the far-reaching extended atmosphere of the sun. Launched in 1997, Voyager 1 is traveling away from Earth at a speed of about 340 million miles (540 million kilometers) per year. In the summer of 2012, Voyager 1 started its journey into interstellar space, or the space between stars. This artist's concept depicts Voyager 1 exiting the heliosphere and entering the interstellar medium (brown hue at the top of the image). When Voyager 1’s Plasma Wave Subsystem detects vibrations it allows scientists to characterize the plasma, or ionized gas, the spacecraft is embedded in. From October to November 2012 and again from April to May 2013, Voyager 1's plasma wave instrument detected vibrations caused by previous explosions on the sun. The inset graph shows the frequency of the waves, which is directly related to the plasma density. The high density clearly indicates that Voyager 1 is embedded in “cold” interstellar plasma, left over from the death of nearby giant stars millions of years ago, which dominates interstellar space. Through extrapolation of measured plasma densities from both events, teams of scientists determined that Voyager 1 first entered interstellar space in the summer of 2012. To listen to the audio version of the oscillations detected by Voyager 1, visit: www.nasa.gov/voyager. Its increasing pitch indicates increasing interstellar plasma density over time.Used in 2014 Calendar. || ",
            "hits": 522
        },
        {
            "id": 11382,
            "url": "https://svs.gsfc.nasa.gov/11382/",
            "result_type": "Produced Video",
            "release_date": "2013-10-30T10:00:00-04:00",
            "title": "Five Years of Great Discoveries for NASA's IBEX",
            "description": "Launched on Oct. 19, 2008, the Interstellar Boundary Explorer, or IBEX, spacecraft, is unique to NASA's heliophysics fleet: it images the outer boundary of the heliosphere, a boundary at the furthest edges of the solar system, far past the planets, some 8 million miles away. There, the constant stream of solar particles flowing off the sun, the solar wind, pushes up against the interstellar material flowing in from the local galactic neighborhood.IBEX is also different because it creates images from particles instead of light. IBEX, scientists create maps from the observed neutral atoms. Some are of non-solar origin, others were created by collisions of solar wind particles with other neutral atoms far from the sun. Observing where these energetic neutral atoms, or ENAs, come from describes what's going on in these distant regions. Over the course of six months and many orbits around Earth, IBEX can paint a picture of the entire sky in ENAs.During its first five years, IBEX has made some astounding discoveries.IBEX is a NASA Heliophysics Small Explorer mission. The Southwest Research Institute in San Antonio, Texas, leads IBEX with teams of national and international partners. NASA's Goddard Space Flight Center in Greenbelt, Md., manages the Explorers Program for the agency's Science Mission Directorate in Washington. || ",
            "hits": 41
        },
        {
            "id": 10908,
            "url": "https://svs.gsfc.nasa.gov/10908/",
            "result_type": "Produced Video",
            "release_date": "2012-05-10T09:00:00-04:00",
            "title": "IBEX: Observing the Sun's Horizon",
            "description": "The Interstellar Boundary Explorer, or IBEX, is the first mission designed to map the entire region of the boundary of our Solar System. As charged particles from the Sun, called the \"solar wind,\" flow outward well beyond the orbits of the planets, they collide with the material between the stars, called the \"interstellar medium\" (ISM). These interactions create energetic neutral atoms (ENAs), particles with no charge that move very quickly. This region emits no light that can be collected by conventional telescopes so, instead, IBEX measures the particles that happen to be traveling inward from the boundary. IBEX contains two detectors designed to collect and measure ENAs, providing data about the mass, location, direction of origin, and energy of these particles. From these data, maps of the boundary are created. IBEX's sole, focused science objective is to discover the nature of the interactions between the solar wind and the interstellar medium at the edge of our Solar System. || ",
            "hits": 62
        },
        {
            "id": 10906,
            "url": "https://svs.gsfc.nasa.gov/10906/",
            "result_type": "Produced Video",
            "release_date": "2012-01-31T13:00:00-05:00",
            "title": "NASA's IBEX Spacecraft Reveals New Observations of Interstellar Matter",
            "description": "A great magnetic bubble surrounds the solar system as it cruises through the galaxy. The sun pumps the inside of the bubble full of solar particles that stream out to the edge until they collide with the material that fills the rest of the galaxy, at a complex boundary called the heliosheath. On the other side of the boundary, electrically charged particles from the galactic wind blow by, but rebound off the heliosheath, never to enter the solar system. Neutral particles, on the other hand, are a different story. They saunter across the boundary as if it weren't there, continuing on another 7.5 billion miles for 30 years until they get caught by the sun's gravity, and sling shot around the star. There, NASA's Interstellar Boundary Explorer lies in wait for them. Known as IBEX for short, this spacecraft methodically measures these samples of the mysterious neighborhood beyond our home. IBEX scans the entire sky once a year, and every February, its instruments point in the correct direction to intercept incoming neutral atoms. IBEX counted those atoms in 2009 and 2010 and has now captured the best and most complete glimpse of the material that lies so far outside our own system. The results? It's an alien environment out there: the material in that galactic wind doesn't look like the same stuff our solar system is made of.More than just helping to determine the distribution of elements in the galactic wind, these new measurements give clues about how and where our solar system formed, the forces that physically shape our solar system, and even the history of other stars in the Milky Way.In a series of science papers appearing in the Astrophysics Journal on January 31, 2012, scientists report that for every 20 neon atoms in the galactic wind, there are 74 oxygen atoms. In our own solar system, however, for every 20 neon atoms there are 111 oxygen atoms. That translates to more oxygen in any given slice of the solar system than in the local interstellar space. For media associated with this release, go to #10905 and #3900. || ",
            "hits": 164
        },
        {
            "id": 10536,
            "url": "https://svs.gsfc.nasa.gov/10536/",
            "result_type": "Produced Video",
            "release_date": "2009-12-02T06:00:00-05:00",
            "title": "Suzaku: Intergalactic Prospector",
            "description": "Recently astronomers used the Suzaku orbiting X-ray observatory, operated jointly by NASA and the Japanese space agency, to discover the largest known reservoir of rare metals in the universe.  Suzaku detected the elements chromium and manganese while observing the central region of the Perseus galaxy cluster. The metallic atoms are part of the hot gas, or \"intergalactic medium,\" that lies between galaxies. Exploding stars, or supernovas, forge the heavy elements. The supernovas also create vast outflows, called superwinds. These galactic gusts transport heavy elements into the intergalactic void. || ",
            "hits": 26
        },
        {
            "id": 10332,
            "url": "https://svs.gsfc.nasa.gov/10332/",
            "result_type": "Produced Video",
            "release_date": "2008-10-22T00:00:00-04:00",
            "title": "Solar Neutral Particles",
            "description": "This animation shows a charged solar particle's path leaving the sun, while following the magnetic field lines out to the heliosheath. The solar particle hits a hydrogen atom, stealing its electron and becoming neutral.  We then follow it until we see it hit one of IBEX's detectors. || ",
            "hits": 36
        },
        {
            "id": 10260,
            "url": "https://svs.gsfc.nasa.gov/10260/",
            "result_type": "Produced Video",
            "release_date": "2008-06-14T00:00:00-04:00",
            "title": "IBEX: Exploring The Edge Of Our Solar System",
            "description": "IBEX is a new NASA mission that will study the interaction between the solar wind and the material beyond our Solar System called the interstellar medium. The solar wind flowing out of the sun inflates a bubble that we call the heliosphere. IBEX's job is to study those boundaries and understand how they really work and tell us how the heliosphere is able to do the important job of protecting us here on Earth as well as astronauts in space from the dangerous galactic cosmic rays.To learn more about IBEX, go to www.nasa.gov/ibex. || ",
            "hits": 91
        },
        {
            "id": 20131,
            "url": "https://svs.gsfc.nasa.gov/20131/",
            "result_type": "Animation",
            "release_date": "2007-12-10T00:00:00-05:00",
            "title": "Interstellar Boundary Explorer (IBEX)",
            "description": "These animations show IBEX and it's two imagers specialized to detect neutral atoms from the solar system's outer boundaries and galactic medium. || ",
            "hits": 56
        },
        {
            "id": 20107,
            "url": "https://svs.gsfc.nasa.gov/20107/",
            "result_type": "Animation",
            "release_date": "2007-08-10T00:00:00-04:00",
            "title": "Journey to the Heliopause",
            "description": "This animation starts at our Sun and quickly zooms out through the solar system to reveal the Heliosphere and the Heliopause where Voyager I passed through in November 2003. || ",
            "hits": 130
        },
        {
            "id": 20108,
            "url": "https://svs.gsfc.nasa.gov/20108/",
            "result_type": "Animation",
            "release_date": "2007-08-08T12:00:00-04:00",
            "title": "Milkyway Galaxy zoom",
            "description": "Starting with a view of our Milky Way galaxy, the orange gas in the animation represents the interstellar medium. The bow shock is created because the heliosphere is moving through like a boat through the water, crashing through the interstellar gases. || ",
            "hits": 125
        },
        {
            "id": 2856,
            "url": "https://svs.gsfc.nasa.gov/2856/",
            "result_type": "Visualization",
            "release_date": "2003-11-11T12:00:00-05:00",
            "title": "Model of the Heliosphere Over the Solar Cycle",
            "description": "This magnetohydrodynamical (MHD) model shows how the heliosphere of the Sun might interact with the local interstellar medium (ISM) over the course of a single 11 year solar cycle.  The sun (and the orbit of the Earth) is located in the tiny blue region in the center.  The ISM is moving from left to right.  The solar wind varies from 400 km/s up to 566 km/s and back down to 400 km/s over the cycle in this particular model.  The colors are logarithmically scaled to represent temperature, with blue around 10,000 Kelvins (in the undisturbed ISM and the region immediately around the Sun) and red over 1,000,000 Kelvins (corresponding to the bow shocked region in the plasma).  The green region around the Sun has a radius that varies between 100-200 Astronomical Units. || ",
            "hits": 70
        }
    ]
}