Literature on which the following results are based:

Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Literature on which the following results are based: Pfrommer, 28, MNRAS, in print, ArXiv:77.1693, Simulating cosmic rays in clusters of galaxies III. Non-thermal scaling relations and comparison to observations Pfrommer, Enßlin, Springel, 28, MNRAS, in print, ArXiv:77.177, Simulating cosmic rays in clusters of galaxies II. A unified scheme for radio halos and relics with predictions of the γ-ray emission Pfrommer, Enßlin, Springel, Jubelgas, and Dolag, 27, MNRAS, 378, 38, Simulating cosmic rays in clusters of galaxies I. Effects on the Sunyaev-Zel dovich effect and the X-ray emission Pfrommer, Springel, Enßlin, Jubelgas 26, MNRAS, 367, 113, Detecting shock waves in cosmological smoothed particle hydrodynamics simulations Enßlin, Pfrommer, Springel, and Jubelgas, 27, A&A, 473, 41, Cosmic ray physics in calculations of cosmological structure formation Jubelgas, Springel, Enßlin, and Pfrommer, A&A, in print, astro-ph/6348, Cosmic ray feedback in hydrodynamical simulations of galaxy formation

Cosmic rays in galaxy clusters Radiative simulations flowchart Physical processes in galaxy clusters High-resolution simulations of galaxy clusters

Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Radiative simulations with cosmic ray (CR) physics

Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Radiative simulations with extended CR physics

1 - - 1 Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Radiative cool core cluster simulation: gas density 1 2 1 1+δgas - -1-1

1 - - 1 Cosmic rays in galaxy clusters Mass weighted temperature 1 Physical processes in galaxy clusters High-resolution simulations of galaxy clusters 8 7 6 Tρgas / ρgas [K] - - 1

Cosmic rays in galaxy clusters 1 - Physical processes in galaxy clusters High-resolution simulations of galaxy clusters - 1 Mach number distribution weighted by ε diss 1 M εdiss/ εdiss - - 1 1

Cosmic rays in galaxy clusters 1 - Physical processes in galaxy clusters High-resolution simulations of galaxy clusters - 1 Mach number distribution weighted by ε CR,inj 1 M εcr,inj / εcr,inj - - 1 1

1 - - 1 Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Mach number distribution weighted by ε CR,inj (q > 3) 1 M εcr,inj / εcr,inj (q > 3) - - 1 1

Cosmic rays in galaxy clusters 1 - Physical processes in galaxy clusters High-resolution simulations of galaxy clusters - 1 CR pressure P CR 1-12 -13-14 PCRρgas / ρgas [erg cm 3 h 2 7 ] - -16-1 -17

Cosmic rays in galaxy clusters 1 - Physical processes in galaxy clusters High-resolution simulations of galaxy clusters - 1 Relative CR pressure P CR /P total 1-1 PCR/Ptot ρgas / ρgas - - 1-2

Cosmic rays in galaxy clusters 4 2-2 Physical processes in galaxy clusters High-resolution simulations of galaxy clusters -4-4 -2 2 4 Relative CR pressure P CR /P total 4 2-1 PCR/Ptot ρgas / ρgas -2-4 -4-2 2 4-2

1 - - 1 1 - - 1 Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters CR electron versus CR proton pressure 1 1-2 PCRe/Ptot ρgas / ρgas -1 PCR/Ptot ρgas / ρgas -3 - - - 1-1 -2 Relative pressure of primary CR electrons. Relative pressure of CR protons.

1 - - 1 1 - - 1 Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Primary versus secondary CR electrons 1 1-1 -2-2 -3 PCRe/Ptot ρgas / ρgas -3-4 -6 PCRe/Ptot ρgas / ρgas - - -7-1 - 1-8 Relative pressure of primary CR electrons. Rel. pressure of secondary CR electrons.

Cosmic rays in galaxy clusters Cosmic rays and radiative processes

Cosmic rays in galaxy clusters Cosmic rays and radiative processes

Cosmic rays in galaxy clusters Cosmic rays and radiative processes

Cosmic rays in galaxy clusters Cosmic rays and radiative processes

1 - - 1 Cosmic rays in galaxy clusters Cosmic web: Mach number 1 M εdiss/ εdiss - - 1 1

1 - - 1 ] Cosmic rays in galaxy clusters Radio web: primary CRe (1.4 GHz) 1-2 -4 S ν,primary [ mjy arcmin -2 h 7 2 - -6-1 -8

1 - - 1 ] Cosmic rays in galaxy clusters Radio web: primary CRe (1 MHz) 1-2 -4 S ν,primary [ mjy arcmin -2 h 7 2 - -6-1 -8

1 - - 1 ] Cosmic rays in galaxy clusters Radio web: primary CRe (1 MHz) 1-2 -4 S ν,primary [ mjy arcmin -2 h 7 2 - -6-1 -8

Cosmic rays in galaxy clusters 1 - - 1 ] Radio web: primary CRe (1 MHz), slower magnetic decline 1-2 -4 S ν,primary [ mjy arcmin -2 h 7 2 - -6-1 -8

Cosmic rays in galaxy clusters Hadronic cosmic ray proton interaction

Cosmic rays in galaxy clusters Cosmic rays and radiative processes

1 - - 1 ] Cosmic rays in galaxy clusters Radio halos: secondary CRe (1 MHz) 1-2 -4 S ν,secondary [ mjy arcmin -2 h 7 3 - -6-1 -8

1 - - 1 ] Cosmic rays in galaxy clusters Radio relics + halos 1 MHz 1-2 -4 S ν,total [ mjy arcmin -2 h 7 3 - -6-1 -8

1 - - 1 Cosmic rays in galaxy clusters Radio relics + halos: spectral index 1 1.4 1.2 α ν 1.1 - - 1 1.

Cosmic rays in galaxy clusters Comparison of simulation vs. observation of A226 Clarke & Enßlin (26) Battaglia et al. (28 in prep.) red/yellow: thermal X-ray emission, blue/contours: 1.4 GHz radio emission with giant radio halo and relic

1 - - 1 Cosmic rays in galaxy clusters Thermal X-ray emission 1-4 -6-7 S X [ erg cm -2 s -1 h 3 ] - -8-1 -9

1 - - 1 ] Cosmic rays in galaxy clusters Hadronic γ-ray emission, E γ > MeV 1-4 - -6-7 -8-9 S γ ( MeV, GeV) [ γ cm -2 s -1 h 7 3-1 -

1 - - 1 ] Cosmic rays in galaxy clusters Inverse Compton emission, E IC > MeV 1-4 - -6-7 -8-9 S IC,total ( MeV, GeV) [ γ s -1 cm -2 h 7 3-1 -

1 - - 1 ] Cosmic rays in galaxy clusters Inverse Compton emission, E IC > kev 1-1 -2 - -3-4 -6 S IC,total ( kev, kev) [ γ s -1 cm -2 h 7 3-1 -7

Summary Cosmic rays in galaxy clusters 1 Characteristics of the CRs in clusters: CR proton pressure: time integrated non-equilibrium activities of clusters, modulated by recent mergers. Primary CR electron pressure: resembles current accretion and merging shocks in the virial regions. 2 Non-thermal cluster emission Unified model for the generation of giant radio halos, radio mini-halos, and relics We predict GLAST to detect ten γ-ray clusters: test of the presented scenario exciting experiments allow a complementary view on structure formation as well as fundamental plasma physics!