A Multidimensional Hydrodynamic Code for Structure Evolution in Cosmology

Quilis, Vicent; Ibáñez, Javier; Sáez, D.

doi:10.1086/177753

Cited by 14 publications

(12 citation statements)

References 25 publications

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“…We use the three‐dimensional Eulerian fixed‐grid hydrodynamical code described by Quilis, Ibáñez & Sáez (1996). The code uses modern high‐resolution shock‐capturing (HRSC) techniques, which are specially designed to integrate hyperbolic systems of equations as the hydrodynamic equations.…”

Section: Simulationsmentioning

confidence: 99%

Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations

Quilis

Bower

Balogh

2001

Monthly Notices of the Royal Astronomical Society

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161

184

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A B S T R A C TWe use a three-dimensional hydrodynamical code to simulate the effect of energy injection on cooling flows in the intracluster medium. Specifically, we compare a simulation of a 10 15 -M ( cluster with radiative cooling only with a second simulation in which thermal energy is injected 31 kpc off-centre, over 64 kpc 3 at a rate of 4:9 Â 10 44 erg s 21 for 50 Myr. The heat injection forms a hot, low-density bubble which quickly rises, dragging behind it material from the cluster core. The rising bubble pushes with it a shell of gas which expands and cools. We find the appearance of the bubble in X-ray temperature and luminosity to be in good qualitative agreement with recent Chandra observations of cluster cores. Toward the end of the simulation, at 600 Myr, the displaced gas begins to fall back toward the core, and the subsequent turbulence is very efficient at mixing the low-and high-entropy gas. The result is that the cooling flow is disrupted for up to , 50 Myr after the injection of energy ceases. Thus this mechanism provides a very efficient method for regulating cooling flows, if the injection events occur with a 1:1 duty cycle.

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Section: Simulationsmentioning

confidence: 99%

Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations

Quilis

Bower

Balogh

2001

Monthly Notices of the Royal Astronomical Society

Self Cite

161

184

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“…The cosmological hydrodynamic equations describing the evolution of the baryonic component (see Peebles, 1980) are solved using a hydro-code based on modern highresolution shock-capturing techniques. This code was described in Quilis et al (1996).…”

Section: Cluster Modelmentioning

confidence: 99%

Gravitational Waves from Galaxy Clusters: A New Observable Effect

Quilis

Ibáñez

Sáez

1998

The Astrophysical Journal

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A rich galaxy cluster showing strong resemblance to the observed ones is simulated. A cold dark matter spectrum, Gaussian statistics, a flat universe, and two components (baryonic gas plus dark matter particles) are considered. We have calculated the gravitational-wave output during the epoch of the fully nonlinear and nonsymmetric cluster evolution. The amplitudes and frequencies of the resulting gravitational waves are estimated. Since frequencies are very small-of the order of 10 Ϫ17 Hz-a complete pulse cannot be observed during an admissible integration time; nevertheless, it is proved that these waves can produce an interesting secular effect, which appears to be observable with current technology.

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“…Eulerian methods have also become quite popular for addressing problems in Newtonian astrophysics (e.g. Fryxell, Müller & Arnett 1989; Cen et al 1990; Bryan et al 1994; Quilis, Ibanez & Saez 1996; Yepes et al 1997; Wada & Norman 1999; Ricker, Dodelson & Lamb 2000), especially in the framework of Adaptive Mesh Refinement (AMR; e.g. Bryan & Norman 1997; Khokhlov 1998; Truelove et al 1998; Fryxell et al 2000; Plewa & Müller 2001; Kravtsov, Klypin & Hoffman 2002; Teyssier 2002; Quilis 2004; Wang, Abel & Zhang 2008).…”

Section: Introductionmentioning

confidence: 99%

Computational Eulerian hydrodynamics and Galilean invariance

Robertson

Kravtsov

Gnedin

et al. 2010

Monthly Notices of the Royal Astronomical Society

110

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Eulerian hydrodynamical simulations are a powerful and popular tool for modelling fluids in astrophysical systems. In this work, we critically examine recent claims that these methods violate Galilean invariance of the Euler equations. We demonstrate that Eulerian hydrodynamics methods do converge to a Galilean‐invariant solution, provided a well‐defined convergent solution exists. Specifically, we show that numerical diffusion, resulting from diffusion‐like terms in the discretized hydrodynamical equations solved by Eulerian methods, accounts for the effects previously identified as evidence for the Galilean non‐invariance of these methods. These velocity‐dependent diffusive terms lead to different results for different bulk velocities when the spatial resolution of the simulation is kept fixed, but their effect becomes negligible as the resolution of the simulation is increased to obtain a converged solution. In particular, we find that Kelvin–Helmholtz instabilities develop properly in realistic Eulerian calculations regardless of the bulk velocity provided the problem is simulated with sufficient resolution (a factor of 2–4 increase compared to the case without bulk flows for realistic velocities). Our results reiterate that high‐resolution Eulerian methods can perform well and obtain a convergent solution, even in the presence of highly supersonic bulk flows.

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A Multidimensional Hydrodynamic Code for Structure Evolution in Cosmology

Cited by 14 publications

References 25 publications

Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations

Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations

Gravitational Waves from Galaxy Clusters: A New Observable Effect

Computational Eulerian hydrodynamics and Galilean invariance

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