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PARTICLE ACCELERATION IN STRONG SHOCKS: INFLUENCE ON THE SUPERNOVA REMNANT EVOLUTION IN RADIO

PARTICLE ACCELERATION IN STRONG SHOCKS: INFLUENCE ON THE SUPERNOVA REMNANT EVOLUTION IN RADIO. Dejan Uro šević Department of Astronomy, Faculty of Mathematics, University of Belgrade VII BSAC, 1- 4 June, 2010, CHEPELARE. particle acceleration. particle acceleration.

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PARTICLE ACCELERATION IN STRONG SHOCKS: INFLUENCE ON THE SUPERNOVA REMNANT EVOLUTION IN RADIO

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  1. PARTICLE ACCELERATION IN STRONG SHOCKS: INFLUENCE ON THE SUPERNOVA REMNANT EVOLUTION IN RADIO Dejan Urošević Department of Astronomy, Faculty of Mathematics, University of Belgrade VII BSAC, 1- 4 June, 2010, CHEPELARE

  2. particle acceleration

  3. particle acceleration • first order Fermi acceleration (“Type A” in Fermi (1949)) ΔE / E ~ v / c

  4. particle acceleration • second order Fermi acceleration (“Type B” in Fermi (1949)) – affirmed in this paper ΔE / E ~ (v / c)2

  5. particle acceleration • Cosmic rays • Ultra-relativistic electrons • Synchrotron emission, gamma-ray emission by inverse Compton scattering and pion decay • SNRs, AGNs

  6. particle acceleration(SNRs and AGNs) • diffuse shock acceleration – first order Fermi acceleration • Bell (1978a,b), Blandford & Ostriker (1978, 1980), Drury (1983a,b), Malkov & Drury (2001)

  7. particle acceleration(SNRs and AGNs) • second order Fermi acceleration – turbulences in downstream region • Scott & Chevalier (1975), Galinsky & Shevchenko (2007)

  8. DSA – diffuse shock acceleration • Microscopic approach (Bell1978a)

  9. DSA – diffuse shock acceleration • Probability of escape at a large distance downstream η= 4 v2/ v v – test particle velocity (v ≈ c) ↓↓ PROBABLE RECROSSING FROM DOWNSTREM TO UPSTREAM scattering induced by magnetic turbulence in downstream region

  10. DSA – diffuse shock acceleration • Scattering in upstream region is induced by turbulence in the form of Alfven waves excited by energetic particles which pass through the shock and attempt to escape upstream (quasi-non-linear effect) ↓↓ RECROSSING FROM UPSTREAM TO DOWNSTREM

  11. DSA – diffuse shock acceleration After N cycles particle is “diffuse shocked” Particle “loses memory” about its initial spectrum

  12. DSA – diffuse shock acceleration Resulting spectrum of the cosmic ray particles in DSA theory is power law: N(E) dE ~ E-μdE, where μ=(2v2+v1)/(v1-v2), for strong non-modified shocks (v1=4v2) μ=2

  13. DSA – diffuse shock acceleration Macroscopic approach (Krymsky 1977, Axford et al. 1977, Blandford & Ostriker 1978) f(t,x,p) - distribution function of the phase space density again the power-law form f(p)~ p-4 for the ideal gas (γ= 5/3), and Mach number M → ∞ ↓↓ N(p)dp = 4πp2f(p)dp

  14. DSA – diffuse shock acceleration MODIFIED SHOCKS Non-linear effects Including of cosmic ray (CR) pressure γ = 4/3 → compression ratio r = 7!!!

  15. DSA - SNRs * SNRs are energetically capable to accelerate CRs by DSA mechanism!!! (Blandford & Ostriker 1978) * Still, the particle injection stays as an open problem

  16. DSA - SNRs Injection (Bell 1978b) →Einj = 4(1/2mpvs2)

  17. DSA - SNRs 4(1/2mpvs2) = 2mec2→ vs ≈ 7000 km/s For SNRs in energy conserving phase, the radio (synchrotron) surface brightness (for vs << 7000 km/s) to diameter relation: Σ~ D-3.5 (Duric & Seaquist 1986)

  18. DSA - SNRs Non-linear kinetic theory for CR acceleration in SNRs (Berezhko & Völk 2004) Modified shocks by CR pressure

  19. DSA - SNRs Early free expansion phase vs≈const, shock is slightly modified (PCR ≈const. → B ≈const.)→ Σ~ D Late free expansion phase, vs≠const, shock is slightly modified (PCR ~ vs + equipartition → B~ vs1/2) → Σ~ D-0.3

  20. DSA - SNRs

  21. DSA - SNRs early energy conserving (Sedov) phase, vs~ D-1.5, shock is significantly modified (PCR ~ vs2 → B~ vs) ↓↓ Σ~ D-4.25 (linear theory Σ~ D-3.5)

  22. DSA - SNRs late energy conserving (Sedov) phase, shock decelerates, DSA and mag. Field amplification are irrelevant (PCR ~ vs2 → B≈ const.) ↓↓ Σ~ D-2

  23. DSA - SNRs Injection (Berezhko & Völk 2004 – B&V)

  24. Conclusions 1. Bell’s and B&V models are not in contradiction (in order of used injection models). 2. Different results for energy conserving phase are relics of different models and using of different assumptions. 3. Bell’s model has physically better foundations.

  25. Future work 1. Free expansion evolution in “Bell’s environment” and corresponding radio evolution – preliminary results: Σ~ Dfor early free expansion 2. Evolution of an SNR in radio – excluding phases of evolution 3. Searching for different injection models

  26. Future work • DSA – diffusion only in pinch angle • second order acceleration – diffusion in velocities ↓↓↓ • modeling of both processes in the same time

  27. Regards from the Belgrade ISM gang!!!!!

  28. THANK YOU VERY MUCH FOR ATTENTION!!!

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