Exploring the role of cosmological shock waves in the Dianoga simulations of galaxy clusters
| Autor: | Veronica Biffi, Vicent Quilis, Stefano Borgani, E. Rasia, Gian Luigi Granato, Klaus Dolag, Susana Planelles, Giuseppe Murante, C. Ragone-Figueroa |
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| Rok vydání: | 2021 |
| Předmět: |
Shock wave
Physics Cosmology and Nongalactic Astrophysics (astro-ph.CO) Structure formation Active galactic nucleus Shock (fluid dynamics) 010308 nuclear & particles physics Star formation Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Supernova Space and Planetary Science 0103 physical sciences Cluster (physics) 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Galaxy cluster Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 507:5703-5719 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stab2436 |
| Popis: | Cosmological shock waves are ubiquitous to cosmic structure formation and evolution. As a consequence, they play a major role in the energy distribution and thermalization of the intergalactic medium (IGM). We analyze the Mach number distribution in the Dianoga simulations of galaxy clusters performed with the SPH code GADGET-3. The simulations include the effects of radiative cooling, star formation, metal enrichment, supernova and active galactic nuclei feedback. A grid-based shock-finding algorithm is applied in post-processing to the outputs of the simulations. This procedure allows us to explore in detail the distribution of shocked cells and their strengths as a function of cluster mass, redshift and baryonic physics. We also pay special attention to the connection between shock waves and the cool-core/non-cool core (CC/NCC) state and the global dynamical status of the simulated clusters. In terms of general shock statistics, we obtain a broad agreement with previous works, with weak (low-Mach number) shocks filling most of the volume and processing most of the total thermal energy flux. As a function of cluster mass, we find that massive clusters seem more efficient in thermalising the IGM and tend to show larger external accretion shocks than less massive systems. We do not find any relevant difference between CC and NCC clusters. However, we find a mild dependence of the radial distribution of the shock Mach number on the cluster dynamical state, with disturbed systems showing stronger shocks than regular ones throughout the cluster volume. Comment: 19 pages, 15 figures, accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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