1. Strong nonresonant amplification of magnetic fields in particle accelerating shocks A. E. Vladimirov, D. C. Ellison, A. M. Bykov Submitted to ApJL

2. In diffusive shock acceleration, the streaming of shock- accelerated particles may induce plasma instabilities. A fast non-resonant instability (Bell 2004, MNRAS) may efficiently amplify short-wavelength modes in fast shocks.

3. We developed a fully nonlinear model* of DSA based on Monte Carlo particle transport Magnetic turbulence, bulk flow, superthermal particles derived consistently with each other * Vladimirov, Ellison & Bykov, 2006. ApJ, v. 652, p.1246; Vladimirov, Bykov & Ellison, 2008. ApJ, v. 688, p. 1084

4. ~p 2 ~l cor ~(W res ) -1 Wavenumber, k Turbulence spectrum, k·W(k) Momentum, p Particle mean free path, (p) Turbulence Particles Our model for particle propagation in strong turbulence interpolates between different scattering regimes in different particle energy ranges.

5. k – wavenumber of turbulent harmonics W(x,k) – spectrum of turbulent fluctuations, (energy per unit volume per unit ∆k). Amplification (  corresponds to Bell’s instability) Dissipation Compression (amplitude) Compression (wavelength) Cascading In this work we ignored compression for clarity (does not affect the qualitatively new results)

6. We study the consequences of two hypotheses: A. No spectral energy transfer (i.e., suppressed cascading),  = 0 B. Fast Kolmogorov cascade,  = W 5/2 k 3/2 ρ -1/2

7. Shock-generated turbulence with NO CASCADING Effective magnetic field B = 1.1·10 -3 G Shocked plasma temperature T = 2.2·10 7 K ~p 2 Trapping

8. Without cascading, Bell’s instability forms a turbulence spectrum with several distinct peaks. The peaks occur due to the nonlinear connection between particle transport and magnetic field amplification. Without a cascade-induced dissipation, the plasma in the precursor remains cold.

9. Shock-generated turbulence with KOLMOGOROV CASCADE Effective magnetic field B = 1.5·10 -4 G Shocked plasma temperature T = 4.4·10 7 K ~p 2 Resonant scattering

10. With fast cascading, Bell’s instability forms a smooth, hard power law turbulence spectrum The effective downstream magnetic field turns out lower with cascading, as well as the maximum particle energy Viscous dissipation of small-scale fluctuations in the process of cascading induces a strong heating of the backround plasma upstream.

11. Summary We studied magnetic field amplification in a nonlinear particle accelerating shock dominated by Bell’s nonresonant short- wavelength instability If spectral energy transfer (cascading) is suppressed, turbulence energy spectrum has several distinct peaks If cascading is efficient, the spectrum is smoothed out, and significant heating increases the precursor temperature Without Cascading With Cascading

12. Discussion With better information about spectral energy transfer ( in a strongly magnetized plasma with ongoing nonresonant magnetic field amplification, accounting for the interactions with streaming accelerated particles ) we can refine our predictions regarding the amount of MFA, maximum particle energy E max, heating and compression in particle accelerating shocks (plasma simulations needed) If peaks do occur, they define a potentially observable spatial scale and an indirect measurement of E max Peaks in the spectrum may help explain the rapid variability of synchrotron X-ray emission* Observations of precursor heating may provide information about the character of spectral energy transfer in the process of MFA * Bykov, Uvarov & Ellison, 2008 (ApJ)

13. Q? A!

14. Plots from the paper (just in case)

15. The following sequence of slides shows how the peaks are formed one by one in the shock precursor. (model A, no cascading)

16. Very far upstream… Solution with NO CASCADING

17. Far upstream… Turbulence amplification Resonance w/particles Solution with NO CASCADING

18. Upstream… Solution with NO CASCADING

19. Particle trapping occured… Solution with NO CASCADING

20. Second peak formed… Solution with NO CASCADING

21. The story repeated… Solution with NO CASCADING

22. And here is the result (downstream)… Solution with NO CASCADING

23. The following sequence of slides shows how the peaks are formed one by one in the shock precursor. (model B, Kolmogorov cascade)

24. Far upstream… Solution with KOLMOGOROV CASCADE

25. Amplification… Solution with KOLMOGOROV CASCADE

26. Cascading forms a k -5/3 power law… Solution with KOLMOGOROV CASCADE

27. Amplification continues in greater k… Solution with KOLMOGOROV CASCADE

28. And a hard spectrum is formed downstream… Solution with KOLMOGOROV CASCADE