Numerical Hydrodynamics in Special Relativity
José María Martí,Ewald Müller +1 more
TLDR
This review is concerned with a discussion of numerical methods for the solution of the equations of special relativistic hydrodynamics (SRHD), and particular emphasis is put on a comprehensive review of the application of high-resolution shock-capturing methods in SRHD.Abstract:
This review is concerned with a discussion of numerical methods for the solution of the equations of special relativistic hydrodynamics (SRHD). Particular emphasis is put on a comprehensive review of the application of high-resolution shock-capturing methods in SRHD. Results obtained with different numerical SRHD methods are compared, and two astrophysical applications of SRHD flows are discussed. An evaluation of the various numerical methods is given and future developments are analyzed.read more
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Smoothed particle hydrodynamics
TL;DR: In this article, the theory and application of Smoothed particle hydrodynamics (SPH) since its inception in 1977 are discussed, focusing on the strengths and weaknesses, the analogy with particle dynamics and the numerous areas where SPH has been successfully applied.
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General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems
TL;DR: In this article, the formation and large-scale propagation of Poynting-dominated jets produced by accreting, rapidly rotating black hole systems are studied by numerically integrating the general relativistic magnetohydrodynamic equations of motion to follow the self-consistent interaction between accretion discs and black holes.
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Rotating Stars in Relativity
TL;DR: The sections on the equilibrium properties and on the nonaxisymmetric instabilities in f-modes and r-Modes have been updated and several new sections have been added on analytic solutions for the exterior spacetime, rotating stars in LMXBs, rotating strange stars, and on rotatingStars in numerical relativity.
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The Einstein Toolkit: A Community Computational Infrastructure for Relativistic Astrophysics
Frank Löffler,Joshua A. Faber,Eloisa Bentivegna,Tanja Bode,Peter Diener,Roland Haas,Roland Haas,Ian Hinder,Bruno C. Mundim,Christian D. Ott,Christian D. Ott,Christian D. Ott,Erik Schnetter,Erik Schnetter,Erik Schnetter,Gabrielle Allen,Gabrielle Allen,Manuela Campanelli,Pablo Laguna +18 more
TL;DR: The Einstein Toolkit as mentioned in this paper is a community-driven, freely accessible computational infrastructure intended for use in numerical relativity, relativistic astrophysics, and other applications, which combines a core set of components needed to simulate astrophysical objects such as black holes, compact objects, and collapsing stars.
Posted Content
Relativistic hydrodynamics
TL;DR: Relativistic hydrodynamics is essential to our current understanding of nucleus-nucleus collisions at ultra-relativists energies as discussed by the authors, and it has been used in a number of experiments at the CERN Large Hadron Collider.
References
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Approximate Riemann Solvers, Parameter Vectors, and Difference Schemes
TL;DR: In this article, it is shown that these features can be obtained by constructing a matrix with a certain property U, i.e., property U is a property of the solution of the Riemann problem.
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Towards the ultimate conservative difference scheme V. A second-order sequel to Godunov's method
TL;DR: In this article, a second-order extension of the Lagrangean method is proposed to integrate the equations of ideal compressible flow, which is based on the integral conservation laws and is dissipative, so that it can be used across shocks.
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Smoothed particle hydrodynamics: Theory and application to non-spherical stars
R. A. Gingold,Joseph J Monaghan +1 more
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Riemann Solvers and Numerical Methods for Fluid Dynamics
TL;DR: In this article, the authors present references and index Reference Record created on 2004-09-07, modified on 2016-08-08 and a reference record created on 2003-09 -07.
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A numerical approach to the testing of the fission hypothesis.
TL;DR: A finite-size particle scheme for the numerical solution of two-and three-dimensional gas dynamical problems of astronomical interest is described and tested in this article, which is then applied to the fission problem for optically thick protostars.