A new general relativistic magnetohydrodynamics code for dynamical spacetimes
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A new general relativistic magnetohydrodynamics code for dynamical spacetimes

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A new general relativistic magnetohydrodynamics code for dynamical spacetimes

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dc.contributor.author Cerdá Durán, Pablo
dc.contributor.author Font Roda, José Antonio
dc.contributor.author Antón Ruiz, Luis
dc.contributor.author Müller, E.
dc.date.accessioned 2010-06-29T11:03:44Z
dc.date.available 2010-06-29T11:03:44Z
dc.date.issued 2008
dc.identifier.uri http://hdl.handle.net/10550/14013
dc.description.abstract We present a new numerical code that solves the general relativistic magneto-hydrodynamical (GRMHD) equations coupled to the Einstein equations for the evolution of a dynamical spacetime within a conformally-flat approximation. This code has been developed with the main objective of studying astrophysical scenarios in which both, high magnetic fields and strong gravitational fields appear, such as the magneto-rotational collapse of stellar cores, the collapsar model of GRBs, and the evolution of neutron stars. The code is based on an existing and thoroughly tested purely hydrodynamical code and on its extension to accommodate weakly magnetized fluids (passive magnetic-field approximation). These codes have been applied in the past to simulate the aforementioned scenarios with increasing levels of sophistication in the input physics. The numerical code we present here is based on high-resolution shock- capturing schemes to solve the GRMHD equations, which are cast in first-order, flux-conservative hyperbolic form, together with the flux constraint transport method to ensure the solenoidal condition of the magnetic field. Since the astrophysical applications envisaged do not deviate significantly from spherical symmetry, the conformal flatness condition approximation is used for the formulation of the Einstein equations; this has repeatedly shown to yield very good agreement with full general relativistic simulations of core- collapse supernovae and the evolution of isolated neutron stars. In addition, the code can handle several equations of state, from simple analytical expressions to microphysical tabulated ones. In this paper we present stringent tests of our new GRMHD numerical code, which show its ability to handle all aspects appearing in the astrophysical scenarios for which the code is intended, namely relativistic shocks, highly magnetized fluids, and equilibrium configurations of magnetized neutron stars. As an application, magneto- rotational core-collapse simulations of a realistic progenitor are presented and the results compared with our previous findings in the passive magnetic-field approximation. en
dc.language.iso en en
dc.relation http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361:200810086&Itemid=129 en
dc.source Cerdá-Durán, P., Font, J. A., Antón, L. and Müller, E. (2008): A new general relativistic magnetohydrodynamics code for dynamical spacetimes, Astronomy and Astrophysics, núm. 492, vol. 3, pp. 937-953 en
dc.subject Gravitation; Hydrodynamics; Magnetohydrodynamics (MHD); Methods : numerical; Relativity; Stars : supernovae : general en
dc.title A new general relativistic magnetohydrodynamics code for dynamical spacetimes en
dc.type info:eu-repo/semantics/article en
dc.type info:eu-repo/semantics/publishedVersion en
dc.subject.unesco UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia::Gravitación en
dc.subject.unesco UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia::Estrellas en
dc.identifier.doi 10.1051/0004-6361:200810086 en
dc.description.private jofontro@uv.es; luis.anton@uv.es en
dc.identifier.idgrec 049673 en

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