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Webb Science Simulations: Planetary Systems and Origins of Life

Supercomputer simulations of planeratry evolution.

Part 1: Turbulent Molecular Cloud Nebula with Protostellar Objects

The 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 Formation

The 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(http://avl.ncsa.illinois.edu/) at NCSA (http://ncsa.illinois.edu/), University of Illinois (www.illinois.edu)

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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    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
Duration: 54.0 seconds
Available formats:
  1280x720 (30 fps) QT         286 MB
  1280x720 (30 fps) QT         154 MB
  960x540 (30 fps) WEBM         3 MB
  320x180     PNG           186 KB
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JWST Science Simulations: Nebula Tour 2 This visualization shows a tour of a turbulent molecular cloud forming multiple protoplanetary disks.  Credits: NCSA, NASA, A. Kritsuk, M. Norman    JWST Science Simulations: Nebula Tour 2

This visualization shows a tour of a turbulent molecular cloud forming multiple protoplanetary disks. Credits: NCSA, NASA, A. Kritsuk, M. Norman
Duration: 50.0 seconds
Available formats:
  1280x720   QT         278 MB
  960x540     WEBM         5 MB
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JWST Science Simulations: Nebula Tour 3. This visualization shows a tour of a turbulent molecular cloud forming multiple protoplanetary disks.  Credits: NCSA, NASA, A. Kritsuk, M. Norman    JWST Science Simulations: Nebula Tour 3.

This visualization shows a tour of a turbulent molecular cloud forming multiple protoplanetary disks. Credits: NCSA, NASA, A. Kritsuk, M. Norman
Duration: 50.0 seconds
Available formats:
  1280x720   QT         225 MB
  960x540     WEBM         4 MB
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JWST Science Simulations: Protoplanetary Disc. This visualization shows a visual tour of a nebula, a turbulent molecular cloud with multiple protostellar objects, to a close-up view of a single protoplanetary disk entering a phase of violent instability, which forms clumps that may become planets or brown dwarfs. Drs. Alexei Kritsuk and Michael Norman provided the computational data of the turbulent molecular cloud.  Dr. Aaron Boley provided the computational data for the isolated protoplanetary disk. The Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk, Michael Norman, and Aaron Boley to visualize and transition between two computational data sets.  AVL rendered the data sets using in-house software.  Credits: NCSA, NASA, A. Kritsuk, M. Norman, A. Boley    JWST Science Simulations: Protoplanetary Disc.

This visualization shows a visual tour of a nebula, a turbulent molecular cloud with multiple protostellar objects, to a close-up view of a single protoplanetary disk entering a phase of violent instability, which forms clumps that may become planets or brown dwarfs. Drs. Alexei Kritsuk and Michael Norman provided the computational data of the turbulent molecular cloud. Dr. Aaron Boley provided the computational data for the isolated protoplanetary disk.

The Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Alexei Kritsuk, Michael Norman, and Aaron Boley to visualize and transition between two computational data sets. AVL rendered the data sets using in-house software. Credits: NCSA, NASA, A. Kritsuk, M. Norman, A. Boley
Duration: 1.1 minutes
Available formats:
  960x720 (29.97 fps) QT         165 MB
  1280x720 (30 fps) QT         144 MB
  1280x720 (30 fps) QT         179 MB
  960x540 (29.97 fps) WEBM         3 MB
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JWST Science Simulations: Solar System Birth. A visualization of the evolution of a young, isolated protoplanetary disk over 16,000 years to study planetary formation.  Credits:  NCSA, NASA, A. Boley    JWST Science Simulations: Solar System Birth.

A visualization of the evolution of a young, isolated protoplanetary disk over 16,000 years to study planetary formation. Credits: NCSA, NASA, A. Boley
Duration: 37.0 seconds
Available formats:
  1920x1080 (29.97 fps) QT         3 GB
  960x720 (29.97 fps) QT         148 MB
  1920x1080 (29.97 fps) QT         724 MB
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Short URL to This Page:http://svs.gsfc.nasa.gov/goto?10662
Animation Number:10662
Completed:2010-09-26
Animators:Donna Cox (AVL NCSA/University of Illinois) (Lead)
 Stuart Levy (AVL NCSA/University of Illinois)
 Matthew Hall (AVL NCSA/University of Illinois)
 Robert Patterson (AVL NCSA/University of Illinois)
 A. J. Christensen (AVL NCSA/University of Illinois)
 Alex Betts (AVL NCSA/University of Illinois)
Producers:Michael McClare (HTSI)
 Donna Cox (AVL NCSA/University of Illinois)
Scientists:Aaron C. Boley (University of Florida)
 Alexei Kritsuk (University of California, San Diego)
 Michael Norman (University of California, San Diego)
Series:Astrophysics Simulations
Goddard TV Tapes:G2010-014 -- JWST Media Resource Reel 2010
 G2010-070 -- JWST Science Animations
Please give credit for this item to:
NASA/Goddard Space Flight Center, the Advanced Visualization Laboratoy at the National Center for Supercomputing Applications, A. Boley, A. Kritsuk and M. Norman
 
Keywords:
SVS >> HDTV
DLESE >> Space science
SVS >> JWST
SVS >> Planets
SVS >> Space
SVS >> Evolution
SVS >> Webb Telescope
SVS >> Star
SVS >> Planetary Science
SVS >> Hydrodynamic Simulation
SVS >> Re-ionization
SVS >> Protoplanetary Disk
SVS >> Molecular Cloud
SVS >> Brown Dwarf
Science paper:On the Density Distribution in Star-forming Interstellar Clouds, Alexei G. Kritsuk, Michael L. Norman, Rick Wagner, APJL submitted 2010 & The Two Modes of Gas Giant Planet Formation, Boley, Aaron C., The Astrophysical Journal Letters, Volume 695, Issue 1, pp. L53-L57 (2009)
 
 


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Many of our multimedia items use the GCMD keywords. These keywords can be found on the Internet with the following citation:
Olsen, L.M., G. Major, K. Shein, J. Scialdone, S. Ritz, T. Stevens, M. Morahan, A. Aleman, R. Vogel, S. Leicester, H. Weir, M. Meaux, S. Grebas, C.Solomon, M. Holland, T. Northcutt, R. A. Restrepo, R. Bilodeau, 2013. NASA/Global Change Master Directory (GCMD) Earth Science Keywords. Version 8.0.0.0.0

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