Turbulence & particle acceleration in galaxy clusters. Gianfranco Brunetti

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1 Turbulence & particle acceleration in galaxy clusters Gianfranco Brunetti

2 Mergers & CR-acceleration Cluster-cluster mergers are the most energetic events in the present Universe (10 64 erg/gyr). They can drive mechanisms for particle acceleration (shocks, turb..) B (1) SHOCKS accelerate CRe ±,CRp (3) e ±, p TURBULENCE reaccelerates fossil CRe ±, CRp and secondaries CRe ± (2) GENERATION OF SECONDARIES p cr p th π 0 γ rays π ± e ± # CRp are constrained by FERMI # Secondaries unlikely to play the major role in RHs # mixture of REACCELERATED primaries & secndaries

3 OUTLINE [common denominator : turbulence/acceleration] Constraints on secondaries/primaries [Jones, Cassano, Zandanel, Oh..] Turbulent acceleration and ICM microphysics [Jones, Ryu, Miniati,..]

4 Pitch-angle isotropy Stochastic REacceleration of primaries & secondaries ICM, B, CRp, CRe Turbulent ACC model Transit Time Damping (TTD) ω-k // v // =0 Brunetti+Lazarian 07 dampings

5 acceleration SECONDARIES time losses acceleration CR protons Brunetti & Blasi 05 Brunetti & Lazarian 11 acceleration PRIMARY electrons time losses Brunetti + 01, Petrosian 01 Brunetti & Lazarian 07 rev: Blasi et al 07; Brunetti & Jones 14 CR Protons: shocks, AGN/galaxies SECONDARIES PRIMARIES: shocks, AGN/galaxies, reconnection seeds

6 Radio & high energies : basic dependences SYNCHROTRON : INVERSE COMPTON : Turb energy flux Into CRe NEUTRAL-PION DECAY : X-RAYS +1

7 Radio & high energies (Brunetti & Lazarian 11) Calculations that consider the general case where both primaries (CRp,CRe) and secondaries (CRe) interact with turbulence (reaccelerated) turbulence Coma f=1 secondaries assumptions E tur 10 % E th E CRp = ~ % E th «B» =0 Π 0 - decay Suzaku NHXM, ASTRO-H Bonafede et al 10 EGRET FERMI Synchrotron ICS turbulence ICS secondaries CTA

8 Constraining secondaries/primaries +1 f= 1 ASTRO-H f=10 f=1 f=10

9 ASTRO-H f= 1 f=10 f=1 f=10 [Cassano s talk] The nature of «seed» electrons determines the jump in radio luminosity (Mpc-scale) between merger and «relaxed» clusters. Gamma-ray LUM decreases with increasing f :

10 Brown et al 11 Stacking of 105 clusters from SUMSS Next generation of radio telescopes The nature of «seeds» electrons determines the level of Mpc-scale radio emission in «relaxed» clusters. f ~1 implies detection of «relaxed» clusters at GHz frequencies via stacking or with the next generation of radiotelescopes. Relaxed clusters less powerful mergers Powerful mergers NOW

11 Brown et al 11 Stacking of 105 clusters from SUMSS Next generation of radio telescopes The nature of «seeds» electrons determines the level of Mpc-scale radio emission in «relaxed» clusters. f ~1 implies detection of «relaxed» clusters at GHz frequencies via stacking or with the next generation of radiotelescopes. Relaxed clusters less powerful mergers Powerful mergers Turbulent models predict radio halos in less powerful mergers that glow up at low radio frequencies (Cassano et al 06, Brunetti et al 08) NOW LOFAR

12 ICM Turbulence :Theoretical (incomplete..) picture (Brunetti & Lazarian 07, Brunetti & Jones 14) Super-Alfvenic Sub-sonic ICM is a weakly collisional and high-beta plasma Fast Modes Slow Modes Modes driven at small scales Reconnection?

13 TTD acceleration (Miller et al 96, Schlickeiser & Miller 98 ICM: Brunetti & Lazarian 07, 11) Transit Time Damping (TTD) ω-k // v // =0 Interaction between magnetic momentm of particles and parallel gradient of B NOTE we use E/B fluctuations *NOT* velocity Prandtl Number k cut ω w > ω ii standard Coulomb ω w < ω ii plasma instabilities MHD model? Cut-off is generated at scales where damping is faster than cascading. Acceleration ultimately depends on damping

14 TTD acceleration (Miller et al 96, Schlickeiser & Miller 98 ICM: Brunetti & Lazarian 07, 11) - Turbulent energy (compressive) - Turbulent (spectrum) - Prandtl/Reynold numbers - Plasma collision frequency - effective mfp/diffusion MHD model? Cut-off is generated at scales where damping is faster than cascading. Acceleration ultimately depends on damping ω w > ω ii standard Coulomb ω w < ω ii plasma instabilities

15 TTD acceleration (Miller et al 96, Schlickeiser & Miller 98 ICM: Brunetti & Lazarian 07, 11) - Turbulent energy (compressive) - Turbulent (spectrum) - Prandtl/Reynold numbers - Plasma collision frequency - effective mfp/diffusion MHD model? Cut-off is generated at scales where damping is faster than cascading. Acceleration ultimately depends on damping ω w > ω ii standard Coulomb ω w < ω ii plasma instabilities Radioelectrons life-time ~ 10 8 yrs

16 Take Home Messages # ORIGIN OF THE RELATIVISTIC ELECTRONS GIANT RADIO HALOS probe particle reacceleration mechanisms that operate on Mpc-scales in merging galaxy clusters. Is this reacceleration of secondaries OR primaries?? Do secondary particles play a significant role in this picture?? Constraints from the «off state» Mpc scale radio emission in relaxed systems Constraints from deeper gamma-ray observations # RADIO HALOS/non-THERMAL EMISSION AS PROBES OF ICM MICROPHYSICS RADIO HALOS probe a hierarchy of processes that operate in the ICM and that drain enery from large-scale motions to electromagnetic fluctuations which in turn scatter/accelerate relativistic particles. These mechanisms operate at scales and in regimes that are crucial for many other problems (heating, transport, etc) and their effectiveness depends on the details of the microphysics of the ICM. Which is the effective particle s mfp in the ICM? Which is the dissipation scale of turbulence in the ICM?

17 Second order FERMI mechanisms In real astrophysical situations both the scale L and the velocity V depend on the turbulent model and on the physics of the interplay between particles and electro-magnetic (electric field) fluctuations. Next viewgraphs will highlight the connection between turbulent acceleration and microphysics of the ICM Transit Time Damping The most efficient mechanism of scattering/acceleration between compressive (MHD) turbulence (long waves) and particles in QLT

18 RECONNECTION? 1 Mpc Owen et al 14 In super-alfvenic turbulence we expect random Scattering with approaching/receding small-scale current sheets : Fermi II like. With possible initial Fermi I «injection». Kowal et al 12 de Gouveia Dalpino et al 03,05 Fermi I mechanisms Lazarian & Vishniac 99

19 Back of the envelope calculations Syn emissivity η CRs η CRe Φ V =0.01 L o =100 kpc δv o =300 km/s

20 Second order FERMI mechanisms In real astrophysical situations both the scale L and the velocity V depend on the turbulent model and on the physics of the interplay between particles and electro-magnetic (electric field) fluctuations. Next viewgraphs will highlight the connection between turbulent acceleration and microphysics of the ICM 2 examples with compressive turbulence (most commonly adpted...so far): Transit Time Damping Stochastic interaction with LS compressions/rarefactions

21 Nonresonant acceleration (Brunetti & Lazarian 07) Relativistic particles diffusing in Compressive turbulence will experience compressions (acceleration) and expansions (deceleration) resulting in a statistical acceleration. Kinetic energy of turbulence Spatial diffusion coefficient due to some process diffusion induced by compressions Spatial diffusion depends on microphysics : scattering with B-fluctuations.

22 Nonresonant acceleration (Brunetti & Lazarian 07) Spectrum: effects Burgers Kolmogorov Kraichnan min scale: effects - Turbulent energy 10kc 100kc - Turbulent scales - CRs diffusion (self-generated, & background turbulence) - Plasma collision frequency (effective mfp)

23 Constraining secondaries/primaries +1 E tur 10 % E th «B» Coma f=1 ASTRO-H

24 Constraining phys parameters Turb energy flux +1 1/3xB f=1 1/3xB f=10 Coma f=1 ASTRO-H ASTRO-H, NuSTAR?: B CTA, Fermi10: CRp, B

25 Constraining phys parameters Turb energy flux +1 1/3xB Coma f=1 ASTRO-H ICS & gamma-rays are boosted up for smaller «B»

26 Magnetic Reconnection & CRs acceleration see Kowal & Lazarian talks Particle acceleration due to Fermi I -like mechanism (de Gouveia dal Pino & Lazarian 03, 05) Multi-islands reconnection (Drake et al 06, 13) Kowal et al 11 Drake et al 13

27 Nonresonant acceleration (Brunetti & Lazarian 07) Kinetic energy of turbulence Spatial diffusion coefficient due to some process diffusion induced by compressions Slow diffusion : Fast diffusion : min scale depends on TTD damping that in turns depends on collisionality/ effective mfp

28 PARTICLES IN A TURBULENT MEDIUM Spatial diffusion via pitchangle scattering δb Resonant & nonresonant interaction between CRs & electromagnetic fluctuations δe Stochastic acceleration (diffusion in particles momentum space)

29 PARTICLES IN A TURBULENT MEDIUM Spatial diffusion via pitchangle scattering δb Resonant & nonresonant interaction between CRs & electromagnetic fluctuations δe Stochastic acceleration (diffusion in particles momentum space) Acceleration via pitch-angle scattering with long MHD waves (ω <Ω/β pl )

30 Focus on CRs (re)acceleration by compressive turbulence (acoustic, fast & slow modes) NON-resonant acceleration mechanisms Collisionless Resonant acceleration mechanisms Transit Time Damping (TTD) ω-k // v // =nώ ω-k // v // =0 Interaction between magnetic momentm of particles and parallel gradient of B TTD is the strongest mechanism operating in ICM conditions (Cassano & Brunetti 05, Brunetti & Lazarian 07)

31 First attempts with SIMULATIONS Donnert et al 13 Donnert & Brunetti 14 Beresnyak et al 13, Miniati 14 ZuHone et al 13

32 Cosmic rays confinement (Voelk et al. 96, Berezinsky et al 97,.. etc ) Resonant scattering with B-fluctuations : gyroresonance D(GeV) cm 2 /s Generation of small scales B-perturbations/waves in the ICM (rev: Brunetti & Jones 14) - Streaming instability (.. Wiener et al 13) - Firehose/mirror instability (.. Brunetti & Lazarian 11, Kunz et al 11) - Gyrokin instability (.. Yan & Lazarian 11)

33 Cosmic rays confinement (Voelk et al. 96, Berezinsky et al 97,.. etc ) Resonant scattering with B-fluctuations : gyroresonance D(GeV) cm 2 /s Generation of small scales B-perturbations/waves in the ICM (rev: Brunetti & Jones 14) - Streaming instability (.. Wiener et al 13) - Firehose/mirror instability (.. Brunetti & Lazarian 11, Kunz et al 11) - Gyrokin instability (.. Yan & Lazarian 11)

34 Radio Halos : are they generated by inefficient mechanism of CRe acceleration? Acceleration time-scale 10 8 years Re-acceleration acceleration losses

35 Cosmic rays confinement (Voelk et al. 96, Berezinsky et al 97) The size of galaxy clusters allows confinement of CRs up to very high energies Time necessary to diffuse on scale = L Spatial diffusion coefficient Escaping from 1 Mpc in few Gyr requires a particles mfp ~ kpc (in our Galaxy the mfp of GeV CRs is 0.01 pc!) CRs diffusion is mediated by scattering with magnetic field fluctuations and the diffusion coefficient depends on the turbulent properties (see Brunetti & Jones 14 for a rev on the ICM)

36 CAVEAT: ANISOTROPIES IN ALFVEN TURBULENCE Anisotropies developed in the turbulent (MHD) cascade strongly reduce the scattering efficiency (Chandran 00 etc etc..) Cho et al 03 Yan & Lazarian 02

37 Fokker-Planck equations in QLT

38 Pitch-angle scattering vs acceleration rough estimate : δb 2 ω-k // v // =nώ rough estimate : Acceleration is a slow process compared to scattering δe 2 Transit Time Damping (TTD) ω-k // v // =0 Interaction btw magnetic moment of particles and parallel gradient of B

39 Cosmic rays confinement (Voelk et al. 96, Berezinsky et al 97,.. etc ) Resonant scattering with B-fluctuations : Blasi, Gabici, Brunetti 07 Brunetti & Jones 14 gyroresonance D(GeV) cm 2 /s Assuming max scales L=100 kpc and δb/b =0.01.

40 Radio Halos : why turbulent reacceleration models started? Evidence of break in the spectrum of the emitting electrons at energies of few GeV τ acc τ loss Re-acceleration acceleration losses

41 Radio Halos : why turbulent reacceleration models started? Acceleration time-scale 10 8 years Re-acceleration acceleration losses

42 Pitch-angle scattering vs acceleration Scattering rough estimate : δb 2 δe 2 rough estimate : Long wavelength MHD waves (ω <Ω/β pl ) Acceleration is a slow process compared to scattering

43 CAVEAT: ANISOTROPIES IN ALFVEN TURBULENCE Anisotropies developed in the turbulent (MHD) cascade strongly reduce the scattering efficiency (Chandran 00 etc etc..) Cho et al 03 Yan & Lazarian 02

44 Brunetti & Lazarian 2011 MNRAS 412, Santos-Lima et al 14

45 RESULTS II : ULTRA-STEEP-SPECTRUM RHs Brunetti & Jones 14 Most of RHs in LOFAR & EMU/WODAN will be «on state» LOFAR T1 is expected to start exploration of «off-state» «off-state» may POTENTIALLY dominate SKA1 surveys Combination of LOFAR & EMU/WODAN efficient for discovery of ultra-steep spectrum : with ½ of RHs in LOFAR T1 ultra-steep

46 Example of particles spectrum (re)acceleration due to Gyroresonance : (Brunetti et al 04) CRe emitting synchrotron in the radio band

47 Effects of the NL interaction of particles-waves on CR evolution Low frequency waves : quasi-isotropic distrib of pitch-angles Gyroresonance ω-k // v // =nώ Transit Time Damping (TTD) ω-k // v // =0 Interaction btw magnetic moment of particles and parallel gradient of B Suitable for ICM! Isotropic fast modes

48 Effects of the NL interaction of particles-waves on CR evolution Low frequency waves : quasi-isotropic distrib of pitch-angles Comment: turbulence in the ICM is a RE-acceleration mechanism rather than an acceleration mechanism Petrosian & East 08

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