Similar to Nat17, but has background pressure perturbations mirroring magnetic perturbations
B ambient = 100
B jet = 10

Left-hand side is the color; Right-hand side is the magnetic field strength

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Time lapse simulation of Magnetic Field Strength of jet with beta = 10

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This is a 512x512 run of the standard MHD Orszag-Tang vortex test with the MHD-TVD solver. It runs for 1 dynamical time. The quantity imaged is density on a scale of 0.1 to 1. This simulation was done by Computational Astrophysics at the University of Minnesota Department of Astronomy. The simulation was done at the Minnesota Supercomputing Institute for Advanced Computational Research. The code is a new version of the MHD-TVD solver of Jones & Ryu, 1995 written by Peter Mendygral.

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This is a model of an non-inflated, buoyant, magnetized bubble moving through a tangled (on large scales), strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an non-inflated, buoyant bubble moving through a tangled (on large scales), strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an non-inflated, buoyant, magnetized bubble moving through a uniform, strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an non-inflated, buoyant bubble moving through a uniform, strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an inflated, buoyant bubble moving through a tangled (on large scales), strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an inflated, buoyant bubble moving through a tangled (on bubble scales), strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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This is a model of an inflated, buoyant bubble moving through a uniform, strong magnetic field in a galaxy cluster. The simulation was performed by Sean O'Neill of Computational Astrophysics at the University of Minnesota using the MHD-TVD code. Details of the calculation appear in O'Neill, De Young, & Jones (2009), available on astro-ph or in an April issue of The Astrophysical Journal.

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