Beyond ideal magnetohydrodynamics: from fibration to 3+1 foliation
Beyond ideal magnetohydrodynamics: from fibration to 3+1 foliation
We consider a resistive multi-fluid framework from the 3 + 1 space-time foliation point-of-view, paying particular attention to issues relating to the use of multi-parameter equations of state and the associated inversion from evolved to primitive variables. We highlight relevant numerical issues that arise for general systems with relative flows. As an application of the new formulation, we consider a three-component system relevant for hot neutron stars. In this case we let the baryons (neutrons and protons) move together, but allow heat and electrons to exhibit relative flow. This reduces the problem to three momentum equations; overall energy-momentum conservation, a generalised Ohm’s law and a heat equation. Our results provide a hierarchy of increasingly complex models and prepare the ground for new state-of-the-art simulations of relevant scenarios in relativistic astrophysics.
Andersson, N.
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Hawke, I.
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Dionysopoulou, K.
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Comer, G.L.
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Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Hawke, I.
fc964672-c794-4260-a972-eaf818e7c9f4
Dionysopoulou, K.
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Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Andersson, N., Hawke, I., Dionysopoulou, K. and Comer, G.L.
(2017)
Beyond ideal magnetohydrodynamics: from fibration to 3+1 foliation.
Classical and Quantum Gravity, 34, [125003].
(doi:10.1088/1361-6382/aa6b39).
Abstract
We consider a resistive multi-fluid framework from the 3 + 1 space-time foliation point-of-view, paying particular attention to issues relating to the use of multi-parameter equations of state and the associated inversion from evolved to primitive variables. We highlight relevant numerical issues that arise for general systems with relative flows. As an application of the new formulation, we consider a three-component system relevant for hot neutron stars. In this case we let the baryons (neutrons and protons) move together, but allow heat and electrons to exhibit relative flow. This reduces the problem to three momentum equations; overall energy-momentum conservation, a generalised Ohm’s law and a heat equation. Our results provide a hierarchy of increasingly complex models and prepare the ground for new state-of-the-art simulations of relevant scenarios in relativistic astrophysics.
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Accepted/In Press date: 4 April 2017
e-pub ahead of print date: 22 May 2017
Organisations:
Mathematical Sciences, Applied Mathematics
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Local EPrints ID: 410918
URI: http://eprints.soton.ac.uk/id/eprint/410918
ISSN: 0264-9381
PURE UUID: c38a901f-2bf8-47a3-9759-a924d56892ea
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Date deposited: 09 Jun 2017 16:31
Last modified: 16 Mar 2024 05:22
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Author:
K. Dionysopoulou
Author:
G.L. Comer
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