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Cosmological Shocks in Eulerian Simulations Main Properties and Cosmic Rays Acceleration.pdf

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Cosmological Shocks in Eulerian Simulations Main Properties and Cosmic Rays Acceleration

a r X i v : 0 8 0 5 .4 2 1 4 v 1 [ a s t r o - p h ] 2 7 M a y 2 0 0 8 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