non thermal activity in clusters of galaxies thermal activity in clusters of galaxies vahe’...
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Non thermal Activity in Clusters of Galaxies
Vahe’ PetrosianCSSA and KIPACStanford UniversityWith: Greg Madejski
Graduate students: Wel Liu, Yanwei Jiang,
Undergraduate students: Kevin Luli, and William East,
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OUTLINE
1. Observations: General
2. Radiation Mechanisms
3. Acceleration Processes
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RXTE Observations of Bullet Cluster
Final, corrected version of the Figure will appear in ApJ Dec. 1, 2006 issuePetrosian, Madejski & Luli 2006)
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Electromagnetic Energy Spectrum in Coma
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Energy Loss Timescale: Cold Plasma
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Timescales For Hot Plasma
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Thermalization Time: POWER LAW TAIL
2/3-38 keV) 20/)(/(10 yr 105.1 kTnrelax ×=τ
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The Required Electron Spectrum
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Predicted Variation of HXR Flux With Redshift
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3. ACCELERATION MECHANISMSGENERAL
A: Electric Fields: Parallel to B Field Parallel to B Field Unstable leads to TURBULENCE
B: Fermi Acceleration1. Shock or Flow Divergence: First Order First Order
Shocks and Scaterers; i.e. TURBULENCE2. Stochastic Acceleration: Second OrderSecond Order
Scat. and Acceleration by TURBULENCE
TURBULENCE
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3. ACCELERATION MECHANISMSGENERAL
A: Electric Fields: Parallel to B Field Parallel to B Field Unstable leads to TURBULENCE
B: Fermi Acceleration1. Shock or Flow Divergence: First Order First Order
Shocks and Scaterers; i.e. TURBULENCE2. Stochastic Acceleration: Second OrderSecond Order
Scat. and Acceleration by TURBULENCE
TURBULENCE
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3B. Particle AccelerationISOTROPIC AND HOMOGENEOUS
shockA+
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Model Parameters
In principle: Density nTemperature TMagnetic Field BScale (geometry) LLevel of Turbulence
or 2)/( BBδ 2)/( soundvvδ
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Kinetic Equation Coefficients
Acceleration rate or time:Loss rate or time:Escape rate or time:Characteristic Times:
acτ
escTlossτ
vLTBB crossep 2/ and )/( 21 ≈Ω∝− δτ
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3. ACCELERATION IN CLUSTERS
1. Steady State Accelerationa. Background thermal particlesb. Injected relativistic particles
2. Time Dependent or Episodica. Background thermal particlesb. Injected Relativistic Particles
General requirements:
relevant for , allfor lossacc EET lossesc τττ <>
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Loss, Scattering, Escape and Acceleration Times
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Loss and Acceleration Times: Turbulence
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3. ACCELERATION IN CLUSTERS
1. Steady State Accelerationa. Background thermal particlesb. Injected relativistic particles
2. Time Dependent or Episodica. Background thermal particlesb. Injected Relativistic Particles
General requirements:
relevant for , allfor lossacc EET lossesc τττ <>
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Spectral Evolution of Injected Power-law: Loss Only
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GAMMA-RAY EMISSION: GLAST
Mechanisms
1. Non-Thermal Bremsstrahlung
2. Inverse Compton of Infrared-OpticalPhotons (Klein-Nishina)
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Energy Loss Timescale: Cold Plasma
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Gamma-ray Emission: Bremsstrahlung
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SUMMARY and CONCLUSIONS
Radio and Hard X-ray(?) Observationsindicate that there are relativistic electrons in several clusters.
This Can Be Explained byepisodic acceleration of injected relativisticelectrons by turbulence and shocks
GLAST (and more hard X-ray) Observations can constrain the radiative and acceleration mechanisms
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2. PLASMA TURBULENCE AND STOCHASTIC ACCELERATION
1. Generation ,1/ >>= νLVeR 1 / >>= ηLVRm
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2. PLASMA TURBULENCE AND STOCHASTIC ACCELERATION
1. Generation2. Cascade: Nonlinear wave-wave int.
,1/ >>>= νLVeR 1 / >>>= ηLVRm
321321 ;)()()( kkkkkk =+=+ ωωω
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2. TURBULENCE CASCADEHD: Large eddies breaking into small onesEddy turnover or cascade time
MHD: Nonlinear wave-wave interactions
Dispersion Relation: (For Low and High Beta Plasmas )
For Alfven, Fast and Slow ModesFor Alfven, Fast and Slow Modes
soundcas VLkkv /)(/1 <≈τ
SoundcasAlfvencas VLVLkkkkkk
/ OR / ;)()()( 321321
≤≤+=+=
ττωωω
soundAlfvenAlfvenSoundAlfven
soundAlfvenSoundAlfvenAlfven
VVVkkVVkkVVVkkVVkk
<=
>=
For , , ,)( For , , ,)(
||||
||||
ω
ω
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2. PLASMA TURBULENCE AND STOCHASTIC ACCELERATION
1. Generation 2. Cascade: Nonlinear wave-wave int.
3. Interactions with Particles: Resonant int.
,1/ >>>= νLVeR 1 / >>>= ηLVRm
321321 ;)()()( kkkkkk =+=+ ωωω
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3. Wave-Particle Interactions
• Dominated by Resonant Interactions
• Lower energy particles interacting with higher wavevectors or frequencies
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2. PLASMA TURBULENCE AND STOCHASTIC ACCELERATION
1. Generation 2. Cascade: Nonlinear wave-wave int.
3. Interactions with Particles: Resonant int.
A. Damping of WavesB. Acceleration of Particles
,1/ >>>= νLVeR 1 / >>>= ηLVRm
321321 ;)()()( kkkkkk =+=+ ωωω
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Dispersion Relation for the Waves(Propagating Along Field Lines)
Plasma Parameter:
Abundances: Electrons, protons and alpha particles
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General Dispersion Relation
Resonance Condition
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3A. TURBULENCE DAMPING
Viscous or Collisional Damping:Collisonless Damping:
Thermal: Heating of PlasmaNonthermal: Particle Acceleration
maxmin
2/11max
)()( where
for damped is Turbulence
kkkRangeInertialkk
kk
casdamp
<<
∝=∝
>−− ττ
Coulk λ<<−1 Coulkl λ>>= −1
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Damping Rate: Fast ModeGeneral Non-thermal Rate
Non-relativistic Limit:
Thermal:
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3A. Turbulence Damping: Low Beta
Parallel (and perpendicular) waves are not damped
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3A. Turbulence Damping: High Beta
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3A. Turbulence Damping High Beta
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kmin
kmax
k-q
k-q’
Turbulence Spectrum
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Magnetic fluctuations in Solar wind
Leamon et al (1998)
Magnetic fluctuations in Solar wind
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Solution of the Wave Equation
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3B. Particle AccelerationISOTROPIC AND HOMOGENEOUS
shockA+
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