Turbulent Motions and Shocks Waves in Galaxy Clusters simulated with AMR

By Franco Vazza, G. Brunetti, Alexei G. Kritsuk, Rick Wagner, Claudio Gheller, M. Norman. 2009

157 citations recorded by the source corpus.

We have implemented an Adaptive Mesh Refinement criterion explicitly designed to increase spatial resolution around discontinuities in the velocity field in ENZO cosmological simulations. With this technique, shocks and turbulent eddies developed during the hierarchical assembly of galaxy clusters are followed with unprecedented spatial resolution, even at large distances from the clusters center. By measuring the spectral properties of the gas velocity field, its time evolution and the properties of shocks for a reference galaxy cluster, we investigate the connection between accretion processes and the onset of chaotic motions in the simulated Inter Galactic Medium over a wide range of scales

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5f51870f47e347b65d539dc55d58fa8ca79c872f

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Citations in the corpus

Moving mesh cosmology: numerical techniques and global statistics (2011, background): “Indeed, a number of numerical studies have analysed turbulence in the intracluster medium (Dolag et al. 2005b; Vazza et al. 2009; Iapichino et al. 2011; Valdarnini 2011).”
Formation of Galaxy Clusters (2012, background): “The left panel of Figure 9 shows these two types of shocks in a map of the shocked cells identified in a cosmological adaptive mesh refinement simulation of a region surrounding a galaxy cluster (from Vazza et al. 2009), along with the gas velocity field.”
Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating (2010, unknown): “…(2005); Dolag et al. (2005); Subramanian et al. (2006); Schekochihin & Cowley (2006); Vazza et al. (2006); Iapichino et al. (2008); Iapichino & Niemeyer (2008); Maier et al. (2009); Battaglia et al. (2009); Vazza et al. (2009); Kuchar & Enßlin (2009); Paul et al. (2011); Schmidt & Federrath (2011).”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, methodology): “In the second method, following previous works on the same topic (e.g. Dolag et al. 2005; Vazza et al. 2006; Vazza et al. 2009; Vazza, Gheller & Brunetti 2010) we mapped the 3–”
The Coma cluster magnetic field from Faraday rotation measures (2009, background): “Furthermore, cosmological numerical simulations have recently demonstrated that 3D power spectrum of the velocity field is well described by a single power law out to at least one virial radius, with a slope very close to the Kolmogor v power law (Vazza et al. 2009a, b).”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “…galaxy clusters for a substantial fraction of the period of cluster-cluster interaction, a few Gyr, possibly driven by shock waves that cross the cluster volume and by the sloshing (and stripping) of cluster cores (e.g., Dolag et al. 2005; Vazza et al. 2009a; Paul et al. 2010; ZuHone et al. 2010).”
Raining on black holes and massive galaxies: the top-down multiphase condensation model (2016, unknown): “This has been corroborated by many computational works in the past decade (e.g. Lau, Kravtsov & Nagai 2009; Vazza et al. 2009; Valdarnini 2011; Gaspari, Brighenti & Temi 2012a; Miniati 2015; Biffi et al. 2016 and references within).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, background): “This kinetic support is largely sourced by infalling and merging structures, which can further generate turbulent gas motions at the boundary between the bulk flow and the thermalized ICM (Dolag et al. 2005; Kim 2007; Vazza et al. 2009).”
Shocking results without shocks: Subsonic turbulence in smoothed particle hydrodynamics and moving-mesh simulations (2011, background): “…find similar or even higher contributions of the kinetic energy in turbulence relative to the thermal energy in the ICM (Iapichino & Niemeyer 2008; Vazza et al. 2009; Maier et al. 2009; Lau et al. 2009; Vazza et al. 2011; Paul et al. 2011; Schmidt & Federrath 2011; Iapichino et al. 2011; Jones et…”