Cosmological Shocks and Cosmic Rays acceleration in Galaxy Clusters by Franco Vazza G.Brunetti C.Gheller IRA-INAF - Univ.Bologna

Shocks should be one of the main ingredient for detected non-thermal emissions in Radio α=2(M2+1)/(M2-1) E Thermal energy After shock: weak shock: ECR/ETH strong shock: ECR/ETH COSMIC RAYS + B field + turbulence R.Halo? Various models: Brunetti et al., Ensslin et al., Blasi et al. .... Relic?

Our SIMULATIONS with ENZO simulations at CINECA & MACH cpu ~ 80 000 h CDM cosmology a total volume of 150Mpc/h

Our SHOCK DETECTING SCHEME SHOCKS FROM VELOCITY JUMPS SMALLER ERRORS AND BETTER RESOLUTION COMPARED TO PREVIOUS DATA

Distribution of Mach numbers at various overdensities cluster shocks are ~0.1% of the total volume, but they contribute to ~30-40% of the total energy Non-collapsed regions clusters filaments outskirts

Evolution with z of the shock population 15Mpc Evolution with z of the shock population

What is the level of the CR injection in our simulations? Jubelgas et al 2006, Gadget-2 simulations clusters filaments

We inject and follow CR in the simulations The motion of the CRs particles in the range 1GeV < ε < 1 TeV and in |B|~ 0.1 – 1μG are advective in simulations diffusion is neglegible tdiff> > v/lcell=tadv advection is not! tadv< tCRp, cool protons tadv~ tCRe, cool leptons

Baryon density Temperature Mach number Cosmic Rays

A LOT of ingredients to model... Direct shock-accelerations Sn/Agn injections Injection of secondary particles Syncrothron losses Turbulent re-accelerations Grazie IC losses