{ "id": 11499, "url": "https://svs.gsfc.nasa.gov/11499/", "page_type": "Produced Video", "title": "Beta Pictoris: Icy Debris Suggests 'Shepherd' Planet", "description": "An international team of astronomers exploring the disk of gas and dust the bright star Beta Pictoris have uncovered a compact cloud of poisonous gas formed by ongoing rapid-fire collisions among a swarm of icy, comet-like bodies. The researchers suggest the comet swarm may be frozen debris trapped and concentrated by the gravity of an as-yet-unseen planet.Using the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile, astronomers mapped millimeter-wavelength light from dust and carbon monoxide (CO) molecules in a disk surrounding the star. Located about 63 light-years away and only 20 million years old, Beta Pictoris hosts one of the closest, brightest and youngest debris disks known, making it an ideal laboratory for studying the early development of planetary systems. The ALMA images reveal a vast belt of carbon monoxide located at the fringes of the system. Much of the gas is concentrated in a single clump located about 8 billion miles (13 billion kilometers) from the star, or nearly three times the distance between the planet Neptune and the sun. The total amount of CO observed, the scientists say, exceeds 200 million billion tons, equivalent to about one-sixth the mass of Earth’s oceans.The presence of all this gas is a clue that something interesting is going on because ultraviolet starlight breaks up CO molecules in about 100 years, much faster than the main cloud can complete a single orbit around the star. Scientists calculate that a large comet must be completely destroyed every five minutes to offset the destruction of CO molecules. Only an unusually massive and compact swarm of comets could support such an astonishingly high collision rate.The researchers think these comet swarms formed when a as-yet-undetected planet migrated outward, sweeping icy bodies into resonant orbits. When the orbital periods of the comets matched the planet's in some simple ratio – say, two orbits for every three of the planet – the comets received a nudge from the planet at the same location each orbit. Like the regular push of a child's swing, these accelerations amplify over time and work to confine the comets in a small region. || ", "release_date": "2014-03-06T14:00:00-05:00", "update_date": "2023-05-03T13:51:06.704856-04:00", "main_image": { "id": 457608, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/Beta_Pic_Reddy_4k_web.jpg", "filename": "Beta_Pic_Reddy_4k_web.jpg", "media_type": "Image", "alt_text": "This artist's concept illustrates the preferred model for explaining ALMA observations of Beta Pictoris. At the outer fringes of the system, the gravitational influence of a hypothetical giant planet (bottom left) captures comets into a dense, massive swarm (right) where frequent collisions occur. The one planet known in the system, Beta Pictoris b, is shown near the star.Credit: NASA's Goddard Space Flight Center/F. Reddy", "width": 320, "height": 180, "pixels": 57600 }, "main_video": { "id": 457590, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/11499_Icy_Disk_H264_Best_1280x720_59.94.mov", "filename": "11499_Icy_Disk_H264_Best_1280x720_59.94.mov", "media_type": "Movie", "alt_text": "Watch: NASA Goddard's Aki Roberge explains how observations with the Atacama Large Millimeter/submillimeter Array in Chile tell us about poison gas, comet swarms, and a hypothetical planet around Beta Pictoris.Credit: NASA's Goddard Space Flight CenterMusic: \"Halos\" by Lars Leonhard, courtesy of the artist and Ultimae Records.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.", "width": 1280, "height": 720, "pixels": 921600 }, "progress": "Complete", "media_groups": [ { "id": 344830, "url": "https://svs.gsfc.nasa.gov/11499/#media_group_344830", "widget": "Basic text with HTML", "title": "", "caption": "", "description": "An international team of astronomers exploring the disk of gas and dust the bright star Beta Pictoris have uncovered a compact cloud of poisonous gas formed by ongoing rapid-fire collisions among a swarm of icy, comet-like bodies. The researchers suggest the comet swarm may be frozen debris trapped and concentrated by the gravity of an as-yet-unseen planet.
Using the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile, astronomers mapped millimeter-wavelength light from dust and carbon monoxide (CO) molecules in a disk surrounding the star. Located about 63 light-years away and only 20 million years old, Beta Pictoris hosts one of the closest, brightest and youngest debris disks known, making it an ideal laboratory for studying the early development of planetary systems.
The ALMA images reveal a vast belt of carbon monoxide located at the fringes of the system. Much of the gas is concentrated in a single clump located about 8 billion miles (13 billion kilometers) from the star, or nearly three times the distance between the planet Neptune and the sun. The total amount of CO observed, the scientists say, exceeds 200 million billion tons, equivalent to about one-sixth the mass of Earth’s oceans.
The presence of all this gas is a clue that something interesting is going on because ultraviolet starlight breaks up CO molecules in about 100 years, much faster than the main cloud can complete a single orbit around the star. Scientists calculate that a large comet must be completely destroyed every five minutes to offset the destruction of CO molecules. Only an unusually massive and compact swarm of comets could support such an astonishingly high collision rate.
The researchers think these comet swarms formed when a as-yet-undetected planet migrated outward, sweeping icy bodies into resonant orbits. When the orbital periods of the comets matched the planet's in some simple ratio – say, two orbits for every three of the planet – the comets received a nudge from the planet at the same location each orbit. Like the regular push of a child's swing, these accelerations amplify over time and work to confine the comets in a small region.", "items": [], "extra_data": {} }, { "id": 344831, "url": "https://svs.gsfc.nasa.gov/11499/#media_group_344831", "widget": "Video player", "title": "", "caption": "", "description": "Watch: NASA Goddard's Aki Roberge explains how observations with the Atacama Large Millimeter/submillimeter Array in Chile tell us about poison gas, comet swarms, and a hypothetical planet around Beta Pictoris.
Credit: NASA's Goddard Space Flight Center
Music: \"Halos\" by Lars Leonhard, courtesy of the artist and Ultimae Records.
Watch this video on the NASA Goddard YouTube channel.
For complete transcript, click here.", "items": [ { "id": 304991, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457598, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/Beta_Pictoris_Diagram_Still.jpg", "filename": "Beta_Pictoris_Diagram_Still.jpg", "media_type": "Image", "alt_text": "Watch: NASA Goddard's Aki Roberge explains how observations with the Atacama Large Millimeter/submillimeter Array in Chile tell us about poison gas, comet swarms, and a hypothetical planet around Beta Pictoris.Credit: NASA's Goddard Space Flight CenterMusic: \"Halos\" by Lars Leonhard, courtesy of the artist and Ultimae Records.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.", "width": 1280, "height": 720, "pixels": 921600 } }, { "id": 304992, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457600, "url": 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explains how observations with the Atacama Large Millimeter/submillimeter Array in Chile tell us about poison gas, comet swarms, and a hypothetical planet around Beta Pictoris.Credit: NASA's Goddard Space Flight CenterMusic: \"Halos\" by Lars Leonhard, courtesy of the artist and Ultimae Records.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.", "width": 1280, "height": 720, "pixels": 921600 } }, { "id": 304982, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457590, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/11499_Icy_Disk_H264_Best_1280x720_59.94.mov", "filename": "11499_Icy_Disk_H264_Best_1280x720_59.94.mov", "media_type": "Movie", "alt_text": "Watch: NASA Goddard's Aki Roberge explains how observations with the Atacama Large Millimeter/submillimeter Array in Chile tell us about poison gas, comet swarms, and a hypothetical planet around Beta Pictoris.Credit: NASA's Goddard Space 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At the outer fringes of the system, the gravitational influence of a hypothetical giant planet (bottom left) captures comets into a dense, massive swarm (right) where frequent collisions occur. The one planet known in the system, Beta Pictoris b, is shown near the star.
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Credit: Univ. of Cambridge/A. Jackson", "items": [ { "id": 305018, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457625, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/85AU4kmps4a-77_dragged_print.jpg", "filename": "85AU4kmps4a-77_dragged_print.jpg", "media_type": "Image", "alt_text": "This animation models the dust produced by a planetary-scale impact involving a Mars-sized body, which is one possible explanation of the gas clump in the Beta Pictoris debris disk. The initial impact places a large amount of debris into orbit around the star, which mostly follows the orbit of the original body (blue circle). After a few thousand years, this has settled into an asymmetric disk with a bright spot at the location of the original impact (blue cross). Collisions between the debris are enhanced at the location of the bright spot, which persists for at least 100,000 years.Credit: Univ. of Cambridge/A. Jackson", "width": 1024, "height": 813, "pixels": 832512 } }, { "id": 305014, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457622, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/85AU4kmps4a.gif", "filename": "85AU4kmps4a.gif", "media_type": "Image", "alt_text": "This animation models the dust produced by a planetary-scale impact involving a Mars-sized body, which is one possible explanation of the gas clump in the Beta Pictoris debris disk. The initial impact places a large amount of debris into orbit around the star, which mostly follows the orbit of the original body (blue circle). After a few thousand years, this has settled into an asymmetric disk with a bright spot at the location of the original impact (blue cross). Collisions between the debris are enhanced at the location of the bright spot, which persists for at least 100,000 years.Credit: Univ. of Cambridge/A. Jackson", "width": 629, "height": 500, "pixels": 314500 } }, { "id": 305016, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457623, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/85AU4kmps4a-77_dragged_web.png", "filename": "85AU4kmps4a-77_dragged_web.png", "media_type": "Image", "alt_text": "This animation models the dust produced by a planetary-scale impact involving a Mars-sized body, which is one possible explanation of the gas clump in the Beta Pictoris debris disk. The initial impact places a large amount of debris into orbit around the star, which mostly follows the orbit of the original body (blue circle). After a few thousand years, this has settled into an asymmetric disk with a bright spot at the location of the original impact (blue cross). Collisions between the debris are enhanced at the location of the bright spot, which persists for at least 100,000 years.Credit: Univ. of Cambridge/A. Jackson", "width": 320, "height": 254, "pixels": 81280 } }, { "id": 305017, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457624, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/85AU4kmps4a.webmhd.webm", "filename": "85AU4kmps4a.webmhd.webm", "media_type": "Movie", "alt_text": "This animation models the dust produced by a planetary-scale impact involving a Mars-sized body, which is one possible explanation of the gas clump in the Beta Pictoris debris disk. The initial impact places a large amount of debris into orbit around the star, which mostly follows the orbit of the original body (blue circle). After a few thousand years, this has settled into an asymmetric disk with a bright spot at the location of the original impact (blue cross). Collisions between the debris are enhanced at the location of the bright spot, which persists for at least 100,000 years.Credit: Univ. of Cambridge/A. Jackson", "width": 960, "height": 540, "pixels": 518400 } }, { "id": 305015, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457621, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/85AU4kmps4a-77_dragged.tiff", "filename": "85AU4kmps4a-77_dragged.tiff", "media_type": "Image", "alt_text": "This animation models the dust produced by a planetary-scale impact involving a Mars-sized body, which is one possible explanation of the gas clump in the Beta Pictoris debris disk. The initial impact places a large amount of debris into orbit around the star, which mostly follows the orbit of the original body (blue circle). After a few thousand years, this has settled into an asymmetric disk with a bright spot at the location of the original impact (blue cross). Collisions between the debris are enhanced at the location of the bright spot, which persists for at least 100,000 years.Credit: Univ. of Cambridge/A. Jackson", "width": 629, "height": 500, "pixels": 314500 } } ], "extra_data": {} }, { "id": 344838, "url": "https://svs.gsfc.nasa.gov/11499/#media_group_344838", "widget": "Video player", "title": "", "caption": "", "description": "This sequence compares images of Beta Pictoris as seen by Hubble in visible light and ALMA. In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. ALMA observes at submillimeter wavelengths, where the star is relatively faint compared to the disk of gas and millimeter-sized dust grains. The location of the star is shown by the asterisk, and the position of the known Jupiter-mass planet is indicated by the cross. The CO gas disk appears slightly inclined to the main disk plane, and the bright clump appears to the right of the star. This gas disk is much larger than our solar system. The source of the Hubble image is here.
Credit: ALMA (ESO/NAOJ/NRAO)/W. Dent and NASA/ESA ", "items": [ { "id": 305020, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457627, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/bpic-ALMA-HST_still.png", "filename": "bpic-ALMA-HST_still.png", "media_type": "Image", "alt_text": "This sequence compares images of Beta Pictoris as seen by Hubble in visible light and ALMA. In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. ALMA observes at submillimeter wavelengths, where the star is relatively faint compared to the disk of gas and millimeter-sized dust grains. The location of the star is shown by the asterisk, and the position of the known Jupiter-mass planet is indicated by the cross. The CO gas disk appears slightly inclined to the main disk plane, and the bright clump appears to the right of the star. This gas disk is much larger than our solar system. The source of the Hubble image is here.Credit: ALMA (ESO/NAOJ/NRAO)/W. Dent and NASA/ESA ", "width": 1281, "height": 958, "pixels": 1227198 } }, { "id": 305022, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457629, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/bpic-ALMA-HST_still_web.jpg", "filename": "bpic-ALMA-HST_still_web.jpg", "media_type": "Image", "alt_text": "This sequence compares images of Beta Pictoris as seen by Hubble in visible light and ALMA. In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. 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In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. ALMA observes at submillimeter wavelengths, where the star is relatively faint compared to the disk of gas and millimeter-sized dust grains. The location of the star is shown by the asterisk, and the position of the known Jupiter-mass planet is indicated by the cross. The CO gas disk appears slightly inclined to the main disk plane, and the bright clump appears to the right of the star. This gas disk is much larger than our solar system. The source of the Hubble image is here.Credit: ALMA (ESO/NAOJ/NRAO)/W. Dent and NASA/ESA ", "width": 1280, "height": 960, "pixels": 1228800 } }, { "id": 305021, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457628, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/bpic-ALMA-HST.mov", "filename": "bpic-ALMA-HST.mov", "media_type": "Movie", "alt_text": "This sequence compares images of Beta Pictoris as seen by Hubble in visible light and ALMA. In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. ALMA observes at submillimeter wavelengths, where the star is relatively faint compared to the disk of gas and millimeter-sized dust grains. The location of the star is shown by the asterisk, and the position of the known Jupiter-mass planet is indicated by the cross. The CO gas disk appears slightly inclined to the main disk plane, and the bright clump appears to the right of the star. This gas disk is much larger than our solar system. The source of the Hubble image is here.Credit: ALMA (ESO/NAOJ/NRAO)/W. Dent and NASA/ESA ", "width": 1280, "height": 960, "pixels": 1228800 } }, { "id": 305023, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 457630, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011499/bpic-ALMA-HST.webmhd.webm", "filename": "bpic-ALMA-HST.webmhd.webm", "media_type": "Movie", "alt_text": "This sequence compares images of Beta Pictoris as seen by Hubble in visible light and ALMA. In the optical image, light from the bright star must be blocked by a disk (circle at center) because it completely saturates the detector in this region. Outside the occulting disk lies an edge-on belt of the finest dust grains, smaller than 1 micron across. ALMA observes at submillimeter wavelengths, where the star is relatively faint compared to the disk of gas and millimeter-sized dust grains. The location of the star is shown by the asterisk, and the position of the known Jupiter-mass planet is indicated by the cross. The CO gas disk appears slightly inclined to the main disk plane, and the bright clump appears to the right of the star. This gas disk is much larger than our solar system. The source of the Hubble image is here.Credit: ALMA (ESO/NAOJ/NRAO)/W. Dent and NASA/ESA ", "width": 960, "height": 540, "pixels": 518400 } } ], "extra_data": {} }, { "id": 344839, "url": "https://svs.gsfc.nasa.gov/11499/#media_group_344839", "widget": "Basic text", "title": "For More Information", "caption": "", "description": "See [http://www.nasa.gov/content/goddard/nearby-stars-icy-debris-suggests-shepherd-planet/](http://www.nasa.gov/content/goddard/nearby-stars-icy-debris-suggests-shepherd-planet/)", "items": [], "extra_data": {} } ], "studio": "GMS", "funding_sources": [ "NASA Astrophysics" ], "credits": [ { "role": "Animator", "people": [ { "name": "Scott Wiessinger", "employer": "USRA" } ] }, { "role": "Video editor", "people": [ { "name": "Scott Wiessinger", "employer": "USRA" } ] }, { "role": "Narrator", "people": [ { "name": "Aki Roberge", "employer": "NASA/GSFC" } ] }, { "role": "Producer", "people": [ { "name": "Scott Wiessinger", "employer": "USRA" } ] }, { "role": "Scientist", "people": [ { "name": "Aki Roberge", "employer": "NASA/GSFC" } ] }, { "role": "Project support", "people": [ { "name": "Aaron E. 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Video credit: NASA's Goddard Space Flight CenterFor complete transcript, click here. || Beta_Pic_Disk_Sim_Still.jpg (1920x1080) [330.2 KB] || Beta_Pic_Disk_Sim_Still_print.jpg (1024x576) [96.2 KB] || Beta_Pic_Disk_Sim_Still_thm.png (80x40) [5.3 KB] || 11896_Beta_Pic_Disk_ProRes_1920x1080_2997.mov (1920x1080) [3.5 GB] || 11896_Beta_Pic_Disk_H264_Best_1920x1080_2997.mov (1920x1080) [2.1 GB] || 11896_Beta_Pic_Disk_H264_Good_1920x1080_2997.mov (1920x1080) [321.8 MB] || 11896_Beta_Pic_Disk_MPEG4_1920X1080_2997.mp4 (1920x1080) [100.6 MB] || G2015-052_Beta_Pic_Disk_Final_appletv.m4v (960x540) [97.4 MB] || G2015-052_Beta_Pic_Disk_Final_1280x720.wmv (1280x720) [109.6 MB] || 11896_Beta_Pic_Disk_H264_Good_1920x1080_2997.webm (1920x1080) [30.4 MB] || G2015-052_Beta_Pic_Disk_Final_appletv_subtitles.m4v (960x540) [97.3 MB] || G2015-052_Beta_Pic_Disk_Final_ipod_lg.m4v (640x360) [41.5 MB] || 11896_Beta_Pictoris_Disk_SRT_Transcript.en_US.srt [5.5 KB] || 11896_Beta_Pictoris_Disk_SRT_Transcript.en_US.vtt [5.5 KB] || G2015-052_Beta_Pic_Disk_Final_ipod_sm.mp4 (320x240) [20.7 MB] || ", "release_date": "2015-06-25T13:00:00-04:00", "update_date": "2023-05-03T13:49:38.857101-04:00", "main_image": { "id": 442845, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011800/a011896/GIF_Still.jpg", "filename": "GIF_Still.jpg", "media_type": "Image", "alt_text": "Loopable video and gif of the simulated Beta Pictoris disk rotated through 360 degreesCredit: NASA Goddard Scientific Visualization Studio", "width": 1080, "height": 1080, "pixels": 1166400 } }, { "id": 11436, "url": "https://svs.gsfc.nasa.gov/11436/", "page_type": "Produced Video", "title": "Disk Detective: Search for Planetary Habitats", "description": "A new NASA-sponsored website, DiskDetective.org, lets the public discover embryonic planetary systems hidden among data from NASA's Wide-field Infrared Survey Explorer (WISE) mission. The site is led and funded by NASA and developed by the Zooniverse, a collaboration of scientists, software developers and educators who collectively develop and manage the Internet's largest, most popular and most successful citizen science projects. WISE, located in Earth orbit and designed to survey the entire sky in infrared light, completed two scans between 2010 and 2011. It took detailed measurements of more than 745 million objects, representing the most comprehensive survey of the sky at mid-infrared wavelengths currently available. Astronomers have used computers to search this haystack of data for planet-forming environments and narrowed the field to about a half-million sources that shine brightly in the infrared, indicating they may be \"needles\": dust-rich circumstellar disks that are absorbing their star's light and reradiating it as heat. Planets form and grow within these disks. But galaxies, interstellar dust clouds, and asteroids also glow in the infrared, which stymies automated efforts to identify planetary habitats. Disk Detective incorporates images from WISE and other sky surveys in the form of brief animations the website calls flip books. Volunteers view a flip book and then classify the object based on simple criteria, such as whether the image is round or includes multiple objects. By collecting this information, astronomers will be able to assess which sources should be explored in greater detail. The project aims to find two types of developing planetary environments. The first, known as young stellar object disks, typically are less than 5 million years old, contain large quantities of gas, and are often found in or near young star clusters. For comparison, our own solar system is 4.6 billion years old. The other type of habitat is called a debris disk. These systems tend to be older than 5 million years, possess little or no gas, and contain belts of rocky or icy debris that resemble the asteroid and Kuiper belts found in our own solar system. Vega and Fomalhaut, two of the brightest stars in the sky, host debris disks. Through Disk Detective, volunteers will help the astronomical community discover new planetary nurseries that will become future targets for NASA's Hubble Space Telescope and its successor, the James Webb Space Telescope. || ", "release_date": "2014-01-30T11:00:00-05:00", "update_date": "2023-05-03T13:51:16.164509-04:00", "main_image": { "id": 459746, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a011400/a011436/Disk_Detective_Still_2.png", "filename": "Disk_Detective_Still_2.png", "media_type": "Image", "alt_text": "Take a tour of DiskDetective.org with Goddard astrophysicist Marc Kuchner, the project's principal investigator.Watch this video on the NASA Goddard YouTube channel.For complete transcript, click here.", "width": 1280, "height": 720, "pixels": 921600 } }, { "id": 10635, "url": "https://svs.gsfc.nasa.gov/10635/", "page_type": "Produced Video", "title": "Dust Simulations Paint Alien's View of the Solar System", "description": "Dust ground off icy bodies in the Kuiper Belt, the cold-storage zone that includes Pluto and millions of other objects, creates a faint infrared disk potentially visible to alien astronomers looking for planets around the sun. Neptune's gravitational imprint on the dust is always detectable in new simulations of how this dust moves through the solar system. By ramping up the collision rate, the simulations show how the distant view of the solar system might have changed over its history. More here. || ", "release_date": "2010-09-23T09:00:00-04:00", "update_date": "2023-05-03T13:54:03.704440-04:00", "main_image": { "id": 490596, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a010600/a010635/Kuiper.jpg", "filename": "Kuiper.jpg", "media_type": "Image", "alt_text": "Short video about the Kuiper Belt and the new supercomputer model of its evolution.For complete transcript, click here.", "width": 1280, "height": 720, "pixels": 921600 } } ], "sources": [], "products": [], "newer_versions": [], "older_versions": [], "alternate_versions": [] }