Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21540404d&link_type=abstract
American Astronomical Society, AAS Meeting #215, #404.04; Bulletin of the American Astronomical Society, Vol. 42, p.225
Astronomy and Astrophysics
Astronomy
Scientific paper
The Cosmos++ general relativistic magnetohydrodynamic code has been further developed to better model the accretion of a magnetically seeded disk onto a Kerr black hole. By altering the tilt of the disk relative to the black hole spin axis, features such as standing shocks and coherent oscillation modes have been observed which are absent in non-tilted simulations. Our motivation in the current work is to study the effects that tilt and spin have upon the formation and orientation of the resulting relativistic plasma jets. The simulation of accretion disks and jets on a spherical-polar type grid has two major impediments: the expected orientation of the jet coincides with the location of the axial singularity and the small zone sizes near the axis requires that the area be under-resolved or excised from the grid in order to guarantee a reasonable timestep constraint. To this end, a cubed sphere grid has been developed that is formed from six independent coordinate patches. Such a grid has no singularities outside of the event horizon and provides convergent resolution of the disk and jets while operating at an allowable timestep. The implementation of the cubed sphere was accompanied by changes to the core magnetohydrodynamic scheme in Cosmos++ -- notably the implementation of a new fully-conservative scheme and the addition of flux-constrained transport -- in order to better model magnetically dominated jets. In this poster, we explain the structure and implementation of the cubed sphere grid and contrast it with a spherical-polar grid. We also present initial test results using the new version of Cosmos++ that are relevant to future simulations of jets from tilted accretion disks.
DuPre William
Fragile P.
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