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Methods to solve the relativistic hydrodynamic equations are a key computational kernel in a large number of astrophysics simulations and are crucial to understanding the electromagnetic signals that originate from the merger of astrophysical compact objects.
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Excitation of MHD modes with gravitational waves: A testbed for numerical codes
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First direct comparison of nondisrupting neutron star-black hole and binary black hole merger simulations
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J. M. Alam, N. K.-R. Kevlahan, and O. V. Vasilyev · 2006
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Relativistic MHD with adaptive mesh refinement
M. Anderson, E. W. Hirschmann, S. L. Liebling, and D. Neilsen · 2006
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Primitive variable solvers for conservative general relativistic magnetohydrodynamics
S. C. Noble, C. F. Gammie, J. C. McKinney, and L. Del Zanna · 2006
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An adaptive wavelet-collocation method for shock computations
J. D. Regele and O. V. Vasilyev · 2009
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Wavelet methods for elliptic partial differential equations
K. Urban · 2009
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Topical Review: Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors
J. Abadie, B. P. Abbott, R. Abbott, M. Abernathy, T. Accadia, F. Acernese, C. Adams, R. Adhikari, P. Ajith, B. Allen, et al · 2010
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Mergers of magnetized neutron stars with spinning black holes: Disruption, accretion and fallback
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Mass ejection from the merger of binary neutron stars
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High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars
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GRHydro: A new open source general-relativistic magnetohydrodynamics code for the Einstein Toolkit
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A numerical approach for solving singular nonlinear Lane-Emden type equations arising in astrophysics
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