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Evolutionary Models of Cold, Magnetized, Interstellar CloudsWe modeled the long-term and small-scale evolution of molecular clouds using direct 2D and 3D magnetohydrodynamic (MHD) simulations. This work followed up on previous research by our group under auspices of the ATP in which we studied the energetics of turbulent, magnetized clouds and their internal structure on intermediate scales. Our new work focused on both global and smallscale aspects of the evolution of turbulent, magnetized clouds, and in particular studied the response of turbulent proto-cloud material to passage through the Galactic spiral potential, and the dynamical collapse of turbulent, magnetized (supercritical) clouds into fragments to initiate the formation of a stellar cluster. Technical advances under this program include developing an adaptive-mesh MHD code as a successor to ZEUS (ATHENA) in order to follow cloud fragmentation, developing a shearing-sheet MHD code which includes self-gravity and externally-imposed gravity to follow the evolution of clouds in the Galactic potential, and developing radiative transfer models to evaluate the internal ionization of clumpy clouds exposed to external photoionizing UV and CR radiation. Gammie's work at UIUC focused on the radiative transfer aspects of this program.
Document ID
20040084064
Acquisition Source
Goddard Space Flight Center
Document Type
Contractor or Grantee Report
Authors
Gammie, Charles F.
(Illinois Univ. Urbana-Champaign, IL, United States)
Ostriker, Eve
(Maryland Univ. College Park, MD, United States)
Stone, James M.
(Princeton Univ. NJ, United States)
Date Acquired
August 21, 2013
Publication Date
June 17, 2004
Subject Category
Astrophysics
Funding Number(s)
CONTRACT_GRANT: NAG5-9180
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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