Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes

By A. Sa̧dowski, Ramesh Narayan, A. Tchekhovskoy, Yucong Zhu. 2012

170 citations recorded by the source corpus.

A numerical scheme is described for including radiation in multi-dimensional generalrelativistic conservative fluid dynamics codes. In this met hod, a covariant form of the M1 closure scheme is used to close the radiation moments, and the radiative source terms are treated semi-implicitly in order to handle both optically t hin and optically thick regimes. The scheme has been implemented in a conservative general relativistic radiation hydrodynamics codeKORAL. The robustness of the code is demonstrated on a number of test problems, including radiative relativistic shock tubes, static radiation p ressure supported atmosphere, shadows, beams of light in curved spacetime, and radiative Bondi accretion. The advantages of M1 closure relative to other approaches such as Eddington closure and flux-limited di ffusion are discussed, and its limitations are also highlighted.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f40ce2711dfbb82324c74c0d1269920ef3266235

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Citations in the corpus

The black hole accretion code (2016, background): “Similar to [60, 77], alongside the usual fluid equations, BHAC can be configured to solve an advection equation for the entropy S”
Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, unknown): “More sophisticated treatment of radiation in the context of thin accretion flows is being developed (e.g. Fragile et al. 2012; Sa̧dowski et al. 2013).”
Magnetic Reconnection and Hot Spot Formation in Black Hole Accretion Disks (2020, background): “In the Standard And Normal Evolution (SANE, Narayan et al. 2012; Sadowski et al. 2013) state a fully turbulent accretion disk can develop due to a smaller magnetic flux (see e.g., Porth et al. 2019), and current sheets can ubiquitously form and interact with the turbulent flow.”
First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring (2019, unknown): “Models with 1f ~ are conventionally referred to as Standard and Normal Evolution (SANE; Narayan et al. 2012; Saḑowski et al (2013a)) models; models with maxf f~ are conventionally referred to as Magnetically Arrested Disk (MAD; Igumenshchev et al. 2003; Narayan et al. 2003) models.”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “This is probably an upper limit (see Narayan et al. 2012; Sa̧dowski et al. 2013b).”
Three-dimensional simulations of supercritical black hole accretion discs - luminosities, photon trapping and variability (2015, methodology): “The simulations described in this paper were performed with the general relativistic radiation magnetohydrodynamical (GRRMHD) code KORAL (Sądowski et al. 2013) which solves the conservation equations in a fixed, arbitrary spacetime using finite-difference methods.”
Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “…might be the consequence of the constrained ability of AEF schemes to correctly describe the superposition of oblique radiation fronts (see, e.g. Sa̧dowski et al. 2013; Skinner & Ostriker 2013 for more comments on this property, which is closely related to what is sometimes called ‘two-beam…”
Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo (2014, methodology): “2.1 GRRMHD code — KORAL We use the general relativistic radiation magnetohydrodynamics (GRRMHD) code KORAL (Sa̧dowski et al. 2013a, 2014), which employs a Godunov scheme to evolve the rest mass, energy and momentum conservation equations in a fixed, arbitrary spacetime using finite-difference…”
The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project (2019, methodology): “In fact, a large simulation library comprising 43 well-resolved GRMHD simulations has been created for comparison to the observations, using iharm3D, KORAL, H-AMR, and BHAC (Event Horizon Telescope Collaboration et al. 2019b).”
Numerical simulations of super-critical black hole accretion flows in general relativity (2013, methodology): “The M1 closure scheme employed here is approximate in the sense that KORAL does not include any frequency dependence, but instead evolves the frequency integrated radiative energy density and flux, with grey opacities.”
First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole (2022, methodology): “…dimensions using multiple algorithms: KHARMA (Prather et al. 2021), BHAC (Porth et al. 2017; Olivares et al. 2019), HAMR (Liska et al. 2019), koral (Sądowski et al. 2013), and Athena++ (White et al. 2016); see Porth et al. (2019) and H. Olivares et al. (2022 in preparation) for comparisons of…”