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P. M. Motl, J. E. Tohline, L Lehner (Louisiana State University)
We present a new numerical code (Flow-er) for calculating astrophysical flows in 1, 2 or 3 dimensions. We have implemented equations appropriate for the treatment of Newtonian gravity as well as the general relativistic formalism to treat flows with either a static or dynamic metric. The heart of the code is the recent non-oscillatory central difference scheme by Kurganov and Tadmor (2000; hereafter KT). With this technique, we do not require a characteristic decomposition or the solution of Riemann problems that are required by most other high resolution, shock capturing techniques. Furthermore, the KT scheme naturally incorporates the Method of Lines, allowing considerable flexibility in the choice of time integrators. We have implemented several interpolation kernels that allow us to choose the spatial accuracy of an evolution. Through the Cactus framework or independent code, Flow-er serves as a driver for the hydrodynamical portion of a simulation utilizing adaptive mesh refinement or on a unigrid. In addition to describing Flow-er, we present results from several test problems. We are pleased to acknowledge support for this work from the National Science Foundation through grants PHY-0326311 and AST-0407070.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.