GRHydro: a new open-source general-relativistic magnetohydrodynamics code for the Einstein toolkit

Mösta, Philipp; Mundim, Bruno C.; Faber, Joshua A.; Haas, Roland; Noble, Scott C.; Bode, Tanja; Löffler, Frank; Ott, Christian D.; Reisswig, Christian; Schnetter, Erik

doi:10.1088/0264-9381/31/1/015005

Cited by 148 publications

(236 citation statements)

References 125 publications

(424 reference statements)

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“…The core of the code used for this work is the Einstein Toolkit [27,28], which is a free, publicly available, community-driven general relativistic (GR) code, capable of performing numerical relativity simulations that include realistic physical treatments of matter, electromagnetic fields [29], and gravity.…”

Section: B Numerical Setup and Evolution Methodsmentioning

confidence: 99%

Stiffness effects on the dynamics of the bar-mode instability of neutron stars in full general relativity

et al. 2015

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We present results on the effect of the stiffness of the equation of state on the dynamical barmode instability in rapidly rotating polytropic models of neutron stars in full General Relativity. We determine the change in the threshold for the emergence of the instability for a range of the adiabatic Γ index from 2.0 to 3.0, including two values chosen to mimic more realistic equations of state at high densities.PACS numbers: 04.25. 04.40.Dg, 95.30.Lz, 97.60.Jd

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Section: B Numerical Setup and Evolution Methodsmentioning

confidence: 99%

Stiffness effects on the dynamics of the bar-mode instability of neutron stars in full general relativity

et al. 2015

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“…The evolution of the hydrodynamics is performed by GRHydro [37,47,48], that solves the general relativistic hydrodynamics equations in flux-conservative form, in the so-called Valencia formulation [49][50][51], using highresolution shock-capturing (HRSC) methods. The GRHD evolutions equations are described in Appendix B.…”

Section: B Matter Evolutionmentioning

confidence: 99%

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

et al. 2016

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In this work we present 3D numerical relativity simulations of thick accretion disks around tilted Kerr black holes. We investigate the evolution of three different initial disk models with a range of initial black hole spin magnitudes and tilt angles. For all the disk-to-black hole mass ratios considered (0.044 − 0.16) we observe significant black hole precession and nutation during the evolution. This indicates that for such mass ratios, neglecting the self-gravity of the disks by evolving them in a fixed background black hole spacetime is not justified. We find that the two more massive models are unstable against the Papaloizou-Pringle (PP) instability and that those PP-unstable models remain unstable for all initial spins and tilt angles considered, showing that the development of the instability is a very robust feature of such PP-unstable disks. Our lightest model, which is the most astrophysically favorable outcome of mergers of binary compact objects, is stable. The tilt between the black hole spin and the disk is strongly modulated during the growth of the PP instability, causing a partial global realignment of black hole spin and disk angular momentum in the most massive model with constant specific angular momentum l. For the model with non-constant lprofile we observe a long-lived m = 1 non-axisymmetric structure which shows strong oscillations of the tilt angle in the inner regions of the disk. This effect might be connected to the development of Kozai-Lidov oscillations. Our simulations also confirm earlier findings that the development of the PP instability causes the long-term emission of large amplitude gravitational waves, predominantly for the l = m = 2 multipole mode. The imprint of the BH precession on the gravitational waves from tilted BH-torus systems remains an interesting open issue that would require significantly longer simulations than those presented in this work.

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“…(ii) Mesh refinement with Carpet (iii) Matter evolution with GRHydro [57] (iv) Metric evolution using McLachlan BSSN evolution of the matrix (v) Initial data computed using the LORENE CODE.…”

Section: Einstein Toolkitmentioning

confidence: 99%

Power-Efficient Computing: Experiences from the COSA Project

Cesini¹,

Corni²,

Falabella³

et al. 2017

Scientific Programming

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Energy consumption is today one of the most relevant issues in operating HPC systems for scientific applications. The use of unconventional computing systems is therefore of great interest for several scientific communities looking for a better tradeoff between time-to-solution and energy-to-solution. In this context, the performance assessment of processors with a high ratio of performance per watt is necessary to understand how to realize energy-efficient computing systems for scientific applications, using this class of processors. Computing On SOC Architecture (COSA) is a three-year project (2015)(2016)(2017) funded by the Scientific Commission V of the Italian Institute for Nuclear Physics (INFN), which aims to investigate the performance and the total cost of ownership offered by computing systems based on commodity low-power Systems on Chip (SoCs) and high energyefficient systems based on GP-GPUs. In this work, we present the results of the project analyzing the performance of several scientific applications on several GPU-and SoC-based systems. We also describe the methodology we have used to measure energy performance and the tools we have implemented to monitor the power drained by applications while running.

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GRHydro: a new open-source general-relativistic magnetohydrodynamics code for the Einstein toolkit

Cited by 148 publications

References 125 publications

Stiffness effects on the dynamics of the bar-mode instability of neutron stars in full general relativity

Stiffness effects on the dynamics of the bar-mode instability of neutron stars in full general relativity

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

Power-Efficient Computing: Experiences from the COSA Project

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