Axisymmetric hydrodynamics in numerical relativity using a multipatch method

Jesse, Jerred; Duez, Matthew D.; Foucart, François; Haddadi, Milad; Knight, Alexander; Cadenhead, Courtney L.; Hébert, François; Kidder, Lawrence E.; Pfeiffer, H. P.; Scheel, Mark A.

doi:10.1088/1361-6382/abbc8b

Cited by 7 publications

(5 citation statements)

References 72 publications

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“…We evolve the relativistic viscous hydrodynamic equations using the Spectral Einstein Code (SpEC) [29] with multipatch methods for 2D axisymmetry as described in [30]. The disk mass is less than a percent of the black hole mass even at the initial time, and the metric is very close to stationary in the merger coordinates, so we keep the spacetime metric fixed throughout the simulations.…”

Section: Hydrodynamics and Handling Of Low Densitiesmentioning

confidence: 99%

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport effects

Haddadi¹,

Duez²,

Foucart³

et al. 2022

Preprint

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Section: Hydrodynamics and Handling Of Low Densitiesmentioning

confidence: 99%

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport effects

Haddadi¹,

Duez²,

Foucart³

et al. 2022

Preprint

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“…We evolve the relativistic viscous hydrodynamic equations using the SpEC [29] with multipatch methods for 2D axisymmetry as described in [30]. (See citeJesse:2020,Duez:2020lgq for tests of our 2D viscous hydrodynamics and neutrino transport codes.)…”

Section: Hydrodynamics and Handling Of Low Densitiesmentioning

confidence: 99%

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport

Haddadi

Duez

Foucart

et al. 2023

Class. Quantum Grav.

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Detectable electromagnetic counterparts to gravitational waves from compact binary mergers can be produced by outflows from the black hole-accretion disk remnant during the first ten seconds after the merger. Two-dimensional axisymmetric simulations with effective viscosity remain an efficient and informative way to model this late-time post-merger evolution. In addition to the inherent approximations of axisymmetry and modeling turbulent angular momentum transport by a viscosity, previous simulations often make other simplifications related to the treatment of the equation of state and turbulent transport effects.In this paper, we test the effect of these modeling choices. By evolving with the same viscosity the exact post-merger initial configuration previously evolved in Newtonian viscous hydrodynamics, we find that the Newtonian treatment provides a good estimate of the disk ejecta mass but underestimates the outflow velocity. We find that the inclusion of heavy nuclei causes a notable increase in ejecta mass. An approximate inclusion of r-process effects has a comparatively smaller effect, except for its designed effect on the composition. Diffusion of composition and entropy, modeling turbulent transport effects, has the overall effect of reducing ejecta mass and giving it a speed with lower average and more tightly-peaked distribution. Also, we find significant acceleration of outflow even at distances beyond 10,000 km, so that thermal wind velocities only asymptote beyond this radius and at somewhat higher values than previously reported.

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“…The equatorial coordinate radius is 0.885κ 1=2 G −1=2 . We first evolve the star on a two-dimensional (2D) grid assuming axisymmetry using the techniques described in our recent paper [46]. We use a 2D Cartesian grid, with vertical and radial cylindrical polar coordinates z and ϖ.…”

Section: A Axisymmetric Heatingmentioning

confidence: 99%

Comparison of momentum transport models for numerical relativity

et al. 2020

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The main problems of nonvacuum numerical relativity, compact binary mergers and stellar collapse, involve hydromagnetic instabilities and turbulent flows, so that kinetic energy at small scales leads to mean effects at large scale that drive the secular evolution. Notable among these effects is momentum transport. We investigate two models of this transport effect, a relativistic Navier-Stokes system and a turbulent mean stress model, that are similar to all of the prescriptions that have been attempted to date for treating subgrid effects on binary neutron star mergers and their aftermath. Our investigation involves both stability analysis and numerical experimentation on star and disk systems. We also begin the investigation of the effects of particle and heat transport on postmerger simulations. We find that correct handling of turbulent heating is crucial for avoiding unphysical instabilities. Given such appropriate handling, the evolution of a differentially rotating star and the accretion rate of a disk are reassuringly insensitive to the choice of prescription. However, disk outflows can be sensitive to the choice of method, even for the same effective viscous strength. We also consider the effects of eddy diffusion in the evolution of an accretion disk and show that it can interestingly affect the composition of outflows.

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Axisymmetric hydrodynamics in numerical relativity using a multipatch method

Cited by 7 publications

References 72 publications

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport effects

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport effects

Late-time post-merger modeling of a compact binary: effects of relativity, r-process heating, and treatment of transport

Comparison of momentum transport models for numerical relativity

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