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

2. 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?

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

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

5. 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

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

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

9. 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

10. Baryon density Temperature Mach number Cosmic Rays

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