Characteristic numerical relativity applied to hydrodynamic studies of neutron stars

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dc.creatorSiebel, F.
dc.creatorFont, J. A.
dc.creatorMueller, E.
dc.creatorPapadopoulos, P.
dc.date2000-11-27
dc.date.accessioned2026-07-07T03:25:26Z
dc.date.available2026-07-07T03:25:26Z
dc.descriptionWe present tests and results of a new axisymmetric, fully general relativistic code capable of solving the coupled Einstein-matter system for a perfect fluid matter field. Our implementation is based on the Bondi metric, by which the spacetime is foliated with a family of outgoing light cones. We use high-resolution shock-capturing schemes to solve the fluid equations. The code can accurately maintain long-term stability of a spherically symmetric, relativistic, polytropic equilibrium model of a neutron star. In axisymmetry, we demonstrate global energy conservation of a perturbed neutron star in a compactified spacetime, for which the total energy radiated away by gravitational waves corresponds to a significant fraction of the Bondi mass.
dc.description10 pages, 6 figures, to appear in the proceedings (electronic version) of the Marcel Grossmann Meeting (MG9)
dc.identifierhttps://arxiv.org/abs/gr-qc/0011096
dc.identifierhttp://arxiv.org/abs/gr-qc/0011096
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/33712
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleCharacteristic numerical relativity applied to hydrodynamic studies of neutron stars
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