Content Contact:
Drs. Cen and Ostriker developed one of the largest cosmological hydrodynamic simulations and computed over 749 gigabytes of raw data at the NCSA in 2005. AVL used Amore software (http://avl.ncsa.illinois.edu/what-we-do/software) to interpolate and render approximately 322 gigabytes of a subset of the computed data. The simulation begins about 20 million years after the Big Bang - about 13.7 billion years ago - and extends until the present day.
AVL(http://avl.ncsa.illinois.edu/) at NCSA (http://ncsa.illinois.edu/), University of Illinois (www.illinois.edu)
This visualization shows small galaxies forming, interacting, and merging to make ever-larger galaxies. This 'hierarchical structure formation' is driven by gravity and results in the creation of galaxies with spiral arms much like our own Milky Way galaxy. The Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics was developed by Drs. Brian O'Shea and Michael Norman. The AMR code generated 1.8 terabytes of data and was computed at NCSA. AVL used Amore software (http://avl.ncsa.illinois.edu/what-we-do/software) to interpolate and render 2700 frames (42 gigabytes of HD images). The simulation spans a time period of 13.7 billion years. This visualization provides insight into the assembly and formation of galaxies. James Webb Space Telescope (JWST) will probe the earliest periods of galaxy formation by looking deep into space to see the first galaxies that form in the universe, only a few hundred million years after the Big Bang.
The Advanced Visualization Laboratory (AVL) at the National Center for Supercomputing Applications (NCSA) collaborated with NASA and Drs. Brian O'Shea and Michael Norman to visualize the formation of a Milky Way-type galaxy.
The Adaptive Mesh Refinement (AMR) simulation generated from ENZO code for cosmology and astrophysics was developed by Drs. Brian O'Shea and Michael Norman. The AMR code generated 1.8 terabytes of data and was computed at NCSA. AVL used Amore software (http://avl.ncsa.illinois.edu/what-we-do/software) to interpolate and render 2700 frames (42 gigabytes of HD images). The simulation spans a time period of 13.7 billion years. This visualization provides insight into the assembly and formation of galaxies. James Webb Space Telescope (JWST) will probe the earliest periods of galaxy formation by looking deep into space to see the first galaxies that form in the universe, only a few hundred million years after the Big Bang.
AVL(http://avl.ncsa.illinois.edu/) at NCSA (http://ncsa.illinois.edu/), University of Illinois (www.illinois.edu)
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.
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.
Webb has been at Goddard in some form for 21 years. And with the completion of the acoustic, vibration and center of curvature tests, the telescope part of the Webb spacecraft was finally ready for the next big test - the cryogenic vacuum test in the Apollo-made-famous Chamber A.
Transporting Webb is a carefully choreographed dance. For the move to Johnson, the telescope was placed into a climate-controlled container called STTARS (Space Telescope Transporter for Air Road and Sea). A truck then slowly moved the large container during the night to Joint Base Andrews where it was loaded into a C-5 cargo airplane. The container is so tall that some power lines and traffic lights were moved.
After a flight to Ellington Field in Houston, Texas, Webb was driven to Johnson.
Webb was unpacked in Houston's Chamber A cleanroom and preparation for testing commenced.
NIRSpec is being built for the European Space Agency (ESA) by the Astrium consortium.
NIRCam was built by the University of Arizona and Lockheed Martin.
NASA and Canadian Space Agency (CSA) engineers install the Fine Guidance Sensor (FGS) / Near-InfraRed Imager and Slitless Spectrograph (NIRISS) instrument package onto the Webb Telescope's Integrated Science Instrument Module (ISIM). The FGS/NIRISS was built by the Canadian Space Agency and delivered to NASA Goddard in July of 2012.
The Fine Guidance Sensor (FGS) allows Webb to point precisely, so that it can obtain high-quality images. The Near Infrared Imager and Slitless Spectrograph part of the FGS/NIRISS will be used to investigate the following science objectives: first light detection, exoplanet detection and characterization, and exoplanet transit spectroscopy. It has a wavelength range of 0.8 to 5.0 microns, and is a specialized instrument with three main modes, each of which addresses a separate wavelength range.