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O. Donmez (NASA/GSFC and Drexel University), J. Centrella (NASA/GSFC), C. Miller (Astronomy Dept., Univ. of MD)
Stellar black hole candidates exhibit a variety of time-varying X-ray emissions from chaotic variations to quasi-periodic oscillations. The origins of these emissions are subjects of active study, and some of them are expected to result from hydrodynamic phenomena in the accretion disks. We have developed a numerical code for simulating fluid flow around a black hole in full general relativity. This code uses adaptive mesh refinement (AMR) to resolve features of varying dynamic range. We will present initial results from this code, and will discuss applications to X-ray timing observations.
The author(s) of this abstract have provided an email address for comments about the abstract: odonmez@milkyway.gsfc.nasa.gov