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Cosmological Shocks in Eulerian Simulations Main Properties and Cosmic Rays Acceleration
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Mem. S.A.It. Vol. , 1
c? SAIt 2008 Memorie dellaCosmologi
al Sho
ks in Eulerian Simulations:Main Properties and Cosmi
Rays A
eleration
F.Vazza
1,2
, G. Brunetti
2
, and C. Gheller
3
1
Dipartimento di Astronomia, Universita? di Bologna, via Ranzani 1,I-40127 Bologna, Italy
2
INAF/Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna
3
CINECA, High Performance System Division, Casalecchio di Reno–Bologna, Italy
Abstract. Aims: morpholgies, number and energy distributions of Cosmological Shock
Waves from a set of ENZO cosmological simulations are produced, along with a study of
the connection with Cosmic Rays processes in different environments. Method: we perform
cosmological simulations with the public release of the PPM code ENZO, adopt a simple
and physically motivated numerical setup to follow the evolution of cosmic structures at the
resolution of 125kpc per cell, and characterise shocks with a new post processing scheme.
Results: we estimate the efficency of the acceleration of Cosmic Ray particles and present
the first comparison of our results with existing limits from observations of galaxy clusters.
Key words. galaxy: clusters, general – methods: numerical – intergalactic medium
1. Introduction
Galaxy clusters store up to several 10
63
ergs
in the form of hot baryonic matter, due to
the action of shock-heating processes in large
scale structures formation (Zel’Dovich, 1970).
Detecting shocks in Large Scale Structures
(LSS) is still observationally challenging since
they should more frequently develop in pe-
ripheral, low X emitting regions of clusters,
due to the drop in the sound speed there (e.g.
Markevitch Vikhlinin 2007). Shocks are im-
portant not only to understand the heating of
the ICM but also because they are expected to
be efficient accelerators of supra–thermal parti-
cles (e.g. Sarazin 1999), which can then be ad-
vected and accumulated inside galaxy cluster
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