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  Encounters of merger and accretion shocks in galaxy clusters and theireffects on intracluster medium

Zhang, C., Churazov, E., Dolag, K., Forman, W. R., & Zhuravleva, I. (2020). Encounters of merger and accretion shocks in galaxy clusters and theireffects on intracluster medium. Monthly Notices of the Royal Astronomical Society, 494(3), 4539-4547. doi:10.1093/mnras/staa1013.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-BC9E-5 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-BC9F-4
Genre: Journal Article

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Zhang, Congyao1, Author              
Churazov, Eugene1, Author              
Dolag, Klaus2, Author              
Forman, William R., Author
Zhuravleva, Irina, Author
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1High Energy Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159881              
2Computational Structure Formation, MPI for Astrophysics, Max Planck Society, ou_2205642              

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 Abstract: Several types/classes of shocks naturally arise during formation and evolution of galaxy clusters. One such class is represented by accretion shocks, associated with deceleration of infalling baryons. Such shocks, characterized by a very high Mach number, are present even in 1D models of cluster evolution. Another class is composed of ‘runaway merger shocks’, which appear when a merger shock, driven by a sufficiently massive infalling subcluster, propagates away from the main-cluster centre. We argue that, when the merger shock overtakes the accretion shock, a new long-living shock is formed that propagates to large distances from the main cluster (well beyond its virial radius), affecting the cold gas around the cluster. We refer to these structures as Merger-accelerated Accretion shocks (MA-shocks) in this paper. We show examples of such MA-shocks in one-dimensioanal (1D) and three-dimensional (3D) simulations and discuss their characteristic properties. In particular, (1) MA-shocks shape the boundary separating the hot intracluster medium (ICM) from the unshocked gas, giving this boundary a ‘flower-like’ morphology. In 3D, MA-shocks occupy space between the dense accreting filaments. (2) Evolution of MA-shocks highly depends on the Mach number of the runaway merger shock and the mass accretion rate parameter of the cluster. (3) MA-shocks may lead to the misalignment of the ICM boundary and the splashback radius.

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 Dates: 2020-04-17
 Publication Status: Published online
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 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa1013
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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 494 (3) Sequence Number: - Start / End Page: 4539 - 4547 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150