The newly imaged disk surrounds SAO 206462, an 8.7-magnitude star located about 456 light-years away in the constellation Lupus. Astronomers estimate that the system is only about 9 million years old. The gas-rich disk spans some 14 billion miles, which is more than twice the size of Pluto's orbit in our own solar system.
The Subaru near-infrared image reveals a pair of spiral features arcing along the outer disk. Theoretical models show that a single embedded planet may produce a spiral arm on each side of a disk. The structures around SAO 206462 do not form a matched pair, suggesting the presence of two unseen worlds, one for each arm.", "items": [], "extra_data": {} }, { "id": 350878, "url": "https://svs.gsfc.nasa.gov/10847/#media_group_350878", "widget": "Video player", "title": "", "caption": "", "description": "Simulations of young stellar systems suggest that planets embedded in a circumstellar disk can produce many distinctive structures, including rings, gaps and spiral arms. This video compares computer simulations of hypothetical systems to the Subaru image of SAO 206462.
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Part 1: Turbulent Molecular Cloud Nebula with Protostellar ObjectsThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk and Michael Norman to visualize a computational data set of a turbulent molecular cloud nebula forming protostellar objects and accretion disks approximately 100 AU in diameter, on the order of the size of our solar system. AVL used its Amore software to interpolate and render the Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics. The AMR simulation was developed by Drs. Kritsuk and Norman at the Laboratory for Computational Astrophysics. The AMR simulation generated more than 2 terabytes of data and follows star formation processes in a self-gravitating turbulent molecular cloud with a dynamic range of half-a-million in linear scale, resolving both the large-scale filamentary structure of the molecular cloud (~5 parsec) and accretion disks around emerging young protostellar objects (down to 2 AU). Part 2: Protoplanetary Disk and Planet FormationThe Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Dr. Aaron Boley to visualize the 16,000 year evolution of a young, isolated protoplanetary disk which surrounds a newly-formed protostar. The disk forms spiral arms and a dense clump as a result of gravitational collapse. Dr. Aaron Boley developed this computational model to investigate the response of young disks to mass accretion from their surrounding envelopes, including the direct formation of planets and brown dwarfs through gravitational instability. The main formation mechanism for gas giant planets has been debated within the scientific community for over a decade. One of these theories is 'direct formation through gravitational instability.' If the self-gravity of the gas overwhelms the disk's thermal pressure and the stabilizing effect of differential rotation, the gas closest to the protostar rotates faster than gas farther away. In this scenario, regions of the gaseous disk collapse and form a planet directly. The study, presented in Boley (2009), explores whether mass accretion in the outer regions of disks can lead to such disk fragmentation. The simulations show that clumps can form in situ at large disk radii. If the clumps survive, they can become gas giants on wide orbits, e.g., Fomalhaut b, or even more massive objects called brown dwarfs. Whether a disk forms planets at large radii and, if so, the number of planets that form, depend on how much of the envelope mass is distributed at large distances from the protostar. The results of the simulations suggest that there are two modes of gas giant planet formation. The first mode occurs early in the disk's lifetime, at large radii, and through the disk instability mechanism. After the main accretion phase is over, gas giants can form in the inner disk, over a period of a million years, through the core accretion mechanism, which researchers are addressing in other studies.Thanks to R. H. Durisen, L. Mayer, and G. Lake for comments and discussions relating to this research. This study was supported in part by the University of Zurich, Institute for Theoretical Physics, and by a Swiss Federal Grant. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.AVL at NCSA, University of Illinois. || ", "release_date": "2021-04-14T00:00:00-04:00", "update_date": "2025-01-06T01:14:37.497133-05:00", "main_image": { "id": 378967, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a010600/a010662/Nebula_Tour_1.00002_print.jpg", "filename": "Nebula_Tour_1.00002_print.jpg", "media_type": "Image", "alt_text": "JWST Science Simulations: Nebula Tour 1.This visualization shows a tour of a turbulent molecular cloud forming multiple protoplanetary disks. Credits: NCSA, NASA, A. Kritsuk, M. Norman", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 10986, "url": "https://svs.gsfc.nasa.gov/10986/", "page_type": "Produced Video", "title": "A Star's Spiral", "description": "NASA-supported researchers using a Japanese telescope in Hawaii have taken the first clear image of a rare sight: a star surrounded by a spiral-armed disk. Telescope images have shown hints of stars with spiral disks before. The clarity of this new image, however, is allowing researchers to study what causes this kind of spiral. Rings called circumstellar disks—composed of gas, dust and an accumulation of small objects—surround some stars. If the ring contains planets, their gravitational pull could alter its circular form and create the spiral arms. These videos take a closer look at the new image of star SAO 206462 and raise the question of whether orbiting planets, or something else entirely, created this curious shape. || ", "release_date": "2012-06-26T00:00:00-04:00", "update_date": "2023-05-03T13:52:59.196552-04:00", "main_image": { "id": 476222, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a010900/a010986/597027main_SAO206462_dust_arms_nolabels_1280x720.jpg", "filename": "597027main_SAO206462_dust_arms_nolabels_1280x720.jpg", "media_type": "Image", "alt_text": "What created the unusual spiral arms surrounding this star?", "width": 1280, "height": 720, "pixels": 921600 } } ], "sources": [], "products": [], "newer_versions": [], "older_versions": [], "alternate_versions": [] }