An efficient shock-capturing central-type scheme for multidimensional relativistic flows. II. Magnetohydrodynamics

By L. Del Zanna, N. Bucciantini, Pasquale Londrillo. 2002

322 citations recorded by the source corpus.

A third order shock-capturing numerical scheme for three-dimensional special relativistic magnetohydrodynamics (3-D RMHD) is presented and validated against several numerical tests. The simple and efficient central scheme described in Paper I (Del Zanna and Bucciantini, Astron. Astrophys., 390, 1177--1186, 2002) for relativistic hydrodynamics is here extended to the magnetic case by following the strategies prescribed for classical MHD by Londrillo and Del Zanna (Astrophys. J., 530, 508--524, 2000). The scheme avoids completely spectral decomposition into characteristic waves, computationally expensive and subject to many degenerate cases in the magnetic case, while it makes use of a two-speed Riemann solver that just require the knowledge of the two local fast magnetosonic velocities. Moreover, the onset of spurious magnetic monopoles, which is a typical problem for multi-dimensional MHD upwind codes, is prevented by properly taking into account the solenoidal constraint and the specific antisymmetric nature of the induction equation. Finally, the extension to generalized orthogonal curvilinear coordinate systems is included, thus the scheme is ready to incorporate general relativistic (GRMHD) effects.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/e2b20898a9221d55a1ef8a29c7c2a452518c8698

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Citations in the corpus

Axially symmetric relativistic MHD simulations of Pulsar Wind Nebulae in Supernova Remnants. On the origin of torus and jet-like features (2004, methodology): “Thanks to the recent progress in numerical relativistic fluid dynamics and MHD (see Del Zanna & Bucciantini 2002; Del Zanna et al. 2003, and references therein), we are now able to start a more quantitative investigation of this problem by means of computer simulations.”
Astrophysical smooth particle hydrodynamics (2009, background): “This test has become a widespread benchmark for relativistic hydrodynamics codes, see for example [224,210,211,225,226].”